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Sample records for coronal estudio retrospectivo

  1. Ameloblastoma en población del noreste de Brasil: un estudio retrospectivo de 60 casos

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    Thiago de Santana Santos

    2010-06-01

    Full Text Available El ameloblastoma es un tumor de epitelio odontogénico, caracterizado por la invasión local y aumento de la tasa de recidiva. Por esto se realizó este estudio descriptivo para determinar el comportamiento de los ameloblastomas en nuestro medio. Método: estudio retrospectivo de 17 años basado en los datos existentes de los archivos del Departamento Oral de Patología. Se analizaron los archivos de pacientes de enero de 1992 a mayo de 2009, con un diagnóstico definitivo de ameloblastoma. Fué recogida la información respecto al sexo, raza, presencia de síntomas, ubicación anatómica y extensión. Resultados: dentro de los 60 pacientes con ameloblastoma se observó, mayor incidencia en la tercera década de vida (28,3 %. Las mujeres fueron más comprometidas que los hombres, con una proporción 1,22:1. La mayoría de lesiones fueron observadas en la raza blanca (51,7 %. El sitio más habitual por la ocurrencia de tumor fue la mandíbula (85 %. Los pacientes fueron sintomáticos en el 75 %. La mayoría de pacientes presentaron lesiones de 3,5 a 6,0 centímetros de extensión (55 %. Conclusiones: el ameloblastoma es mayormente observado en mujeres, en la tercera década de la vida y en la mandíbula. Las diferencias con otros estudios entre el sexo, la edad, raza, extensión, localización anatómica y los síntomas pueden ser atribuidos a las diferencias geográficas.

  2. Estudio retrospectivo de la ocurrencia de accidente cerebrovascular en pacientes diabéticos

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    Elsa Rosa Neira Sanchez

    2000-04-01

    Full Text Available Objetivo: Determinar la frecuencia de diabetes mellitus en la población hospitalizada por ACV, describir las características clínicas del ACV en pacientes diabéticos y no diabéticos y determinar la presencia de otros factores de riesgo para ACV en pacientes diabéticos. Material y Métodos: Es un estudio retrospectivo que incluye pacientes hospitalizados con diagnóstico al alta de ACV, a los que se aplicaron criterios de selección para definir ACV y Diabetes Mellitus. Resultados: La prevalencia del ACV tipo isquémico fue mayor en los pacientes diabéticos que en los no diabéticos (83% vs. 57%, p<0.005. De los pacientes diabéticos, 11 de ellos fueron diagnosticados en el momento de la hospitalización, de los 30 pacientes con diagnóstico previo de esta patología el 33% tenían de 10 a 15 años de diagnóstico de diabetes y 24% tenían más de 15 años de enfermedad. La mayoría de pacientes diabéticos eran portadores de nefropatía diabética (73%y retinopatía diabética (46%. La hipertensión arterial fue 1.2 veces más frecuente en los pacientes diabéticos que en los no diabéticos. También se encontraron más alteraciones en el perfil lipídico de los pacientes diabéticos. Conclusiones: El 15% de la población con ACV tuvo diagnóstico de Diabetes Mellitus. El ACV tipo isquémico fue mas frecuente en los pacientes diabéticos. En los pacientes diabéticos el ACV ocurre mas frecuentemente en aquellos con mas de diez años de enfermedad en los que la diabetes contribuye a aumentar el daño vascular, pero además presentan otras patologías que contribuyen a este daño, como hipertensión arterial, enfermedad cardiovascular y dislipidemias. ( Rev Med Hered 2000; 11:54-61 .

  3. Fracturas en prótesis híbrida implantosoportada. Estudio retrospectivo

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    Ventura de la Torre, Javier

    2014-01-01

    Texto completo descargado desde Teseo INTRODUCCIÓN Es un hecho conocido que el descubrimiento de la osteointegración se produjo de forma fortuita durante unas investigaciones que comenzaron a realizarse en 1952 con estudios microscópicos in situ de la médula ósea del peroné de conejo . A comienzo de los años 60, para seguir la evolución de la médula y el hueso se implantaron cámaras de titanio, en lugar de las de tantalio que normalmente se utilizaban, porque parecía tener unas mejor...

  4. Relevancia clínica de la interacción de la warfarina y del acetaminofén: estudio de cohortes retrospectivo

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    Mauricio Ceballos; César A. González; Héctor A. Holguín; Pedro Amariles

    2016-01-01

    Objetivo: Evaluar el uso concomitante de la warfarina y el acetaminofén en una población ambulatoria de pacientes anticoagulados, como posible factor de riesgo en el aumento de la Relación Normalizada Internacional (INR). Métodos: Estudio de cohortes retrospectivo. Se analizó la información de 1.458 pacientes anticoagulados con la warfarina. El factor de riesgo fue la utilización conjunta de warfarina-acetaminofén; el tiempo de seguimiento fue de 1 mes y como evento final se consideró un i...

  5. Los implantes MG-OSSEOUS: Estudio multicéntrico retrospectivo MG-OSSEOUS implants: A multicentric retrospective study

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    E. Serrano Caturla

    2006-12-01

    Full Text Available Objetivo. Aportar unos datos estadísticamente fiables sobre la supervivencia e incidencias asociadas a los implantes y prótesis del modelo MG-OSSEOUS (Mozo-Grau, S.L., Valladolid, España y demostrar que su eficacia es comparable a todas las marcas comerciales. Material y método. Estudio multicéntrico retrospectivo coordinado por la empresa Scientific Management in O&SS (Barcelona, España. Se colocaron 1001 implantes en 247 pacientes y se diseñaron 328 prótesis, entre los años 2004 y 2005, con un seguimiento de 2 años. Todos los implantes cargados. Se analizan y pormenorizan todos los implantes, por diámetros, longitudes, posiciones, fases quirúrgicas, cargas, tipos y modelos de prótesis y técnicas complementarias aplicadas, tanto sincrónica como anacrónicamente. Resultados. Tras la homogeneización de las muestras, se objetiva una supervivencia del 97,8% a los 2 años, detallando los fracasos según las características de cada caso clínico. No se reporta ningún fracaso de la prótesis. Discusión. Protocolizamos una serie de criterios e indicaciones a la hora de colocar los implantes MG-OSSEOUS según los casos clínicos. Comparamos nuestros resultados con la bibliografía, tanto pretérita como actual, coincidiendo con la manera de actuar a lo largo de la historia de la implantología. Finalmente, extrapolamos los resultados que consideramos comparables a los publicados por el grupo Branemark. Conclusión. La calidad del implante MG-OSSEOUS combinada con protocolos implantológicos científicamente contrastados, muestra un 2,2% de fracaso a los 2 años de seguimiento, con un porcentaje de éxito del 100% tanto en la recolocación del implante como en la fase protésica.Objective. We present some statistically contrasted results regarding the survival and incidences of MG-OSSEOUS implants and prosthetic components (Mozo-Grau, S.L., Valladolid, Spain, and we prove that they have the same efficacy when compared with other

  6. La polémica sobre las lumbalgias y su relación con el trabajo: estudio retrospectivo en trabajadores con invalidez

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    Noriega-Elío Mariano

    2005-01-01

    Full Text Available La lumbalgia es un padecimiento de alta prevalencia en la población trabajadora mexicana y tiene repercusiones económico-sociales de enorme alcance. Las cifras oficiales muestran que por lo menos entre el 10,0 y 15,0% de los dictámenes de invalidez se deben a ella. Este dictamen se otorga sólo cuando se ha demostrado que la enfermedad no tuvo relación con el trabajo. Sin embargo, esta investigación muestra que existe tal relación. El estudio fue retrospectivo y se consideraron a todos los trabajadores con dictamen de invalidez por lumbalgia (210 casos, en un hospital del IMSS de la Ciudad de México, durante un periodo de 7 años. Los resultados muestran la asociación e interacciones entre la lumbalgia invalidante y variables laborales como: puesto de trabajo, antigüedad, esfuerzo físico y levantamiento de cargas. Se discute sobre las dificultades y la precisión diagnósticas de la lumbalgia, así como sobre la causalidad del síndrome. Se sugieren algunas vías clínicas, epidemiológicas y legales para su estudio y prevención.

  7. La polémica sobre las lumbalgias y su relación con el trabajo: estudio retrospectivo en trabajadores con invalidez

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    Mariano Noriega-Elío

    Full Text Available La lumbalgia es un padecimiento de alta prevalencia en la población trabajadora mexicana y tiene repercusiones económico-sociales de enorme alcance. Las cifras oficiales muestran que por lo menos entre el 10,0 y 15,0% de los dictámenes de invalidez se deben a ella. Este dictamen se otorga sólo cuando se ha demostrado que la enfermedad no tuvo relación con el trabajo. Sin embargo, esta investigación muestra que existe tal relación. El estudio fue retrospectivo y se consideraron a todos los trabajadores con dictamen de invalidez por lumbalgia (210 casos, en un hospital del IMSS de la Ciudad de México, durante un periodo de 7 años. Los resultados muestran la asociación e interacciones entre la lumbalgia invalidante y variables laborales como: puesto de trabajo, antigüedad, esfuerzo físico y levantamiento de cargas. Se discute sobre las dificultades y la precisión diagnósticas de la lumbalgia, así como sobre la causalidad del síndrome. Se sugieren algunas vías clínicas, epidemiológicas y legales para su estudio y prevención.

  8. Estudio retrospectivo de masas cutáneas neoplásicas en caninos diagnosticadas histopatológicamente en la Universidad de La Salle (1999-2003

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    Carlos Eduardo Aparicio Ortiz

    2008-12-01

    Full Text Available El propósito del trabajo fue realizar un análisis retrospectivo de las neoplasias cutáneas en caninos diagnosticadas en la Universidad de La Salle, en Bogotá, en el período 1999-2003. El presente estudio se llevó a cabo con la información obtenida de los registros del área diagnóstica e histopatológica de la Universidad de La Salle. La información fue discriminada y analizada teniendo en cuenta las siguientes variables: diagnóstico, raza, sexo, edad, malignidad y localización del tumor. Los 192 casos de pacientes abordados en el estudio fueron agrupados de acuerdo con las neoplasias con el fin de determinar las características y el comportamiento de dichas patologías. La edad promedio de los pacientes fue de 6,5 años, la raza más afectada el Bóxer con el 19,1% (32 perros, seguido del Labrador con un 13% (26 perros y el Caniche con un 10,5% (22 perros; los pacientes machos fueron los más afectados con un 58% (107 perros. Se reveló la gran incidencia del tumor de células de mast (26,2% en el 2003 y 20% en el 2002 y el histiocitoma (12,3% en el 2003 y 10% en el año 2002. Entre otras neoplasias que se observaron de forma recurrente en el estudio se destacan el lipoma, tricoepitelioma, carcinoma de células escamosas y papilomatosis.

  9. La demanda hotelera en España: estudio retrospectivo de la década 1990-2000

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    Fernando Garrigós Simón

    2002-01-01

    Full Text Available El presente estudio pretende realizar un análisis de los principales factores determinantes de la demanda turística a nivel mundial y su evolución, con especial incidencia en la relación entre las motivaciones de los turistas y su concreción en demanda efectiva. Además, el trabajo realiza un análisis descriptivo de cómo algunos de estos factores han influido en el comportamiento de la demanda hotelera española en la última década. Tras el estudio hemos corroborado la importancia de la elasticidad de la demanda hotelera española a factores como la renta o las situaciones políticas internacionales. A su vez hemos observado la evolución de la demanda hacia una mayor preferencia por la calidad, así como el proceso de transformación de esta hacia nuevos segmentos. Finalmente, el análisis de la estacionalidad ha remarcado los efectos de la especialización de nuestra demanda en el segmento de sol y playa y en los mercados de España, Gran Bretaña y Alemania.

  10. Proyecto Wernicke-Semi: Estudio multicéntrico y retrospectivo sobre la encefalopatía de Wernicke

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    Antonio Javier Chamorro Fernández

    2012-09-01

    Full Text Available La encefalopatía de Wernicke (EW es una patología neuropsiquiátrica aguda o subaguda debida al déficit de tiamina y que clásicamente se caracteriza por la presencia de confusión mental, oftalmoplejía y ataxia de lamarcha. Existen numerosas áreas de incertidumbre desde los puntos devista epidemiológico, clínico, diagnóstico y terapéutico, motivos por los quese ha diseñado un estudio multicéntrico dentro del grupo de trabajo de Alcohol y Alcoholismo de la Sociedad Española de Medicina Interna (SEMIque trate de dilucidar estos aspectos.

  11. TABAQUISMO Y RIESGO CORONARIO EN LA POBLACIÓN DE UN CENTRO DE SALUD. ESTUDIO DE COHORTES RETROSPECTIVO

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    Lourdes Cañón-Barroso

    2017-01-01

    Full Text Available El tabaquismo es un importante factor de riesgo para múltiples enfermedades crónicas, tales como enfermedades cardiovasculares y cáncer, y también de muerte prematura. El objetivo fue valorar la relación entre tabaquismo y riesgo coronario total en una cohorte de pacientes de 35 a 74 años de edad. Métodos. Estudio observacional de una cohorte retrospectiva de 1.011 pacientes (edad media 55,7 años, 56,0% mujeres sin antecedentes de enfermedades cardiovasculares, seguidos durante 10 años en un centro de salud de Badajoz (Extremadura, España. Se realizó un análisis multivariante mediante regresión logística binaria, incluyéndose como variable dependiente la incidencia de eventos coronarios durante el periodo de seguimiento. Resultados. El 29,1% de la población era fumadora, con menor edad (52,1 vs 57,2 años, p<0,001, menores cifras de colesterol-HDL (45,7 vs 54,0 mg/dl, p<0,001, menor prevalencia de hipertensión arterial (46,9% vs 61,5%, p<0,01 y obesidad (25,5% vs 31,8%, p=0,055 que los pacientes no fumadores. Sin embargo, durante el seguimiento presentaron mayores tasas de mortalidad (11,2% vs 6,7%, p<0,05 e incidencia de eventos coronarios totales (14,3% vs 9,2%, p<0,05. En el análisis multivariante solamente la edad y el tabaquismo se comportaron como variables predictoras de eventos coronarios totales, correspondiendo al tabaquismo las mayores odds ratio (OR: 2,33; IC95%:1,31-4,16; p<0,01. Conclusiones. En personas de 35 a 74 años seguidos durante 10 años el consumo de tabaco duplica el riesgo de eventos coronarios.

  12. Superior mesenteric venous thrombosis: a retrospective study of thirteen cases Trombosis de vena mesentérica superior: estudio retrospectivo de trece casos

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    S. Muñoz

    2004-06-01

    universitario de Madrid. Diseño experimental: estudio retrospectivo descriptivo. Se revisaron las historias clínicas de los pacientes ingresados en nuestro hospital entre enero de 1998 y diciembre de 2002 con este diagnóstico. Los datos fueron procesados mediante el programa informático SPSS vs. 11. Pacientes: los trece pacientes diagnosticados de TVMS en ese periodo fueron incluidos. Resultados: los factores de riesgo asociados fueron patología tumoral (5, patología aguda intraabdominal (2, poliglobulia (1, mutación del gen de la protrombina (1 y anticuerpos anticardiolipina (1. En 3 pacientes no se encontró factor predisponente. La presentación clínica de todos los pacientes fue dolor abdominal, siendo las náuseas y vómitos el segundo síntoma en frecuencia (7. El diagnóstico se obtuvo por TC abdominal (9, arteriografía (2, ecografía (1 y por histología tras resección intestinal (1. Se realizó anticoagulación aislada en 4 pacientes y anticoagulación más cirugía en 5 casos. En 4 no se realizó tratamiento específico por tratarse de pacientes paliativos debido a la patología de base. Cinco pacientes fallecieron, cuatro de ellos presentaban neoplasia como factor asociado. La mortalidad fue de 38,5%. Conclusiones: la TVMS es una entidad muy poco frecuente, asociada en muchos casos patología neoplásica, lo que influye en su elevada mortalidad. Por la inespecificidad de los síntomas las pruebas de imagen son esenciales para el diagnóstico y para detectar factores asociados. En nuestra serie el TC fue la prueba más rentable.

  13. Estudio retrospectivo de la prevalencia de Fasciola hepática y análisis de pérdidas causadas por decomisos de hígados a nivel de centro de faenamiento

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    Buestán Sarmiento, Priscila Estefanía

    2017-01-01

    Este estudio determinó la prevalencia de Distomatosis hepática en bovinos y porcinos causada por el parásito trematodo Fasciola hepática, y estableció las pérdidas económicas ocasionadas por decomisos de hígados post faenamiento; mediante un análisis económico de pérdidas y un estudio retrospectivo de los años 2015 y 2016 a través de la información de los Registros Mensuales de Inspección Veterinaria que maneja el Centro de faenamiento. This study determined the prevalence of hepatic disto...

  14. Acute hepatitis C in Spain: a retrospective study of 131 cases Hepatitis aguda C en España: estudio retrospectivo de 131 casos

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    Ramón Pérez-Álvarez

    2012-01-01

    Full Text Available Background and aims: the management of acute hepatitis C (AHC is controversial. We have conducted a retrospective study to determine the epidemiological and biochemical aspects, the genotypes, the spontaneous clearance of HCV (SVC, and the treatment responses in patients with AHC. Methods: we have retrospectively collected data from 131 patients with AHC from 18 Spanish hospitals. Results: the mean age was 43 ± 16 years (17-83, 69% were symptomatic. The causes of infection were nosocomial in 40% and intravenous drug users in 20%. Eighty two percent had genotype 1. The delay from symptoms-onset to HCV-RNA confirmation was 50 ± 68 days (range, 11-350 days and to treatment (in 59% 14 ±13 weeks (range, 2-58 days. In the treated group, 80% achieved sustained virological response (SVR versus 57% SVC in untreated patients (p = 0.004. Up to 96% of those treated within the first 12 weeks had SVR versus 86% of those treated later (p = 0.04. Patients with HCV-RNA(- at week 4 resolved with or without treatment more frequently than those HCV-RNA(+ (98 versus 69%, p = 0.005. The treatment was not beneficial if HCV-RNA was undetectable at week 12. No differences in SVR were found in genotype 1 patients treated for 24 or 48 weeks. Patients with low baseline viral load achieved higher SVC and SVR. The SVC in patients with bilirubin > 5 mg/dl was 78 versus 40% in those with lower values (p = 0.004. Conclusions: the most common transmission route was nosocomial. SVR was higher in patients treated than SVC in non-treated. Early treatment (before week 12 achieved the highest response rate. SVC and SVR were more common in patients with a low baseline viral load. Undetectable HCV-RNA at week 4 was associated with high SVR and SVC rates. Jaundice was related with SVC.Introducción y objetivos: el manejo de la hepatitis aguda C (HAC es objeto de controversia. Hemos realizado un estudio prospectivo para conocer los aspectos epidemiológicos, bioquímicos, los

  15. Serviço de Emergência Psiquiátrica em hospital geral: estudo retrospectivo Servicio de emergencia psiquiátrica en hospital general: estudio retrospectivo Emergency psychiatric service in general hospitals: a retrospective study

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    Fernando Sérgio Pereira de Sousa

    2010-09-01

    Full Text Available O Serviço de Emergência Psiquiátrica em Hospital Geral (SEPHG é uma proposta articulada com o movimento da reforma psiquiátrica. Objetivou-se caracterizar os clientes com sofrimento psíquico assistidos no SEPHG Dr. Estevam, em Sobral-CE. Este é um estudo do tipo documental, com abordagem quantitativa, envolvendo 191 clientes atendidos no SEPHG no período de janeiro a dezembro de 2007. Os dados foram coletados a partir de um livro de registro, cujas informações nele contidas foram retiradas dos prontuários dos clientes. Observou-se predomínio de pacientes do sexo masculino (70,15%, com idade entre 30-49 anos (48,71% e solteiros (74,86%. A maioria era proveniente da cidade de Sobral (69,64 %. Em 42,40% dos casos, o diagnóstico foi transtorno do uso de álcool. Grande parte da clientela (66,50% deu entrada no serviço por demanda espontânea. Após avaliação do SEPHG, 43,45% desses clientes foram encaminhados ao CAPS-ad. Pelos resultados, depreende-se o quão imprescindíveis são os serviços de saúde mental.El Servicio de Emergencia Psiquiátrica en Hospital General (SEPHG es una propuesta vinculada al movimiento de la reforma psiquiátrica. Se objetivó caracterizar a los pacientes con trastornos psiquiátricos atendidos en el SEPHG Dr. Estevam, en Sobral-Ceará-Brasil. Estudio de tipo documental con abordaje cualitativa, involucrando 191 pacientes atendidos en el SEPHG entre enero y diciembre de 2007. Los datos fueron recogidos a partir de un libro de registro, cuyas informaciones fueron extraídas de las historias clínicas de los pacientes. Se observó prevalencia de pacientes de sexo masculino (70,15%, con edad entre 30-49 años (48,71% y solteros (74,86%. La mayoría provenía de la ciudad de Sobral (69,64%. En el 42,40% de los casos, el diagnóstico fue trastorno provocado por abuso de alcohol. Una gran cantidad de pacientes (66,50% se presentó en el servicio en forma espontánea. Con posterioridad a la evaluación del

  16. Incidência de cirurgia cardíaca em octogenários: estudo retrospectivo Incidencia de cirugía cardíaca en octogenarios: estudio retrospectivo Incidence of cardiac surgery in octogenarian patients: retrospective study

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    Luciano Brandão Machado

    2003-09-01

    Full Text Available JUSTIFICATIVA E OBJETIVOS: O aumento da expectativa de vida faz com que pacientes cada vez mais idosos tenham indicação de tratamento cirúrgico de cardiopatias. Este estudo tem como objetivo avaliar a incidência de pacientes com mais de 80 anos submetidos à cirurgia cardíaca no Instituto do Coração do Hospital das Clínicas da FMUSP, nos últimos 16 anos. MÉTODO: Foram analisados, no período de 1986 a 2001, o número de cirurgias de revascularização do miocárdio (RM e cirurgia valvar (CV e, em cada grupo, o número de cirurgias em pacientes com mais de 80 anos. Os dados foram analisados descritivamente. RESULTADOS: Os dados revelam aumento progressivo do número de octogenários submetidos à cirurgia cardíaca. As cirurgias de revascularização do miocárdio tiveram aumento de 0,13% em 1986 para 3,5% em 2001. As cirurgias valvares aumentaram de 0% em 1986 para 1,44% em 2001, registrando o maior valor de 3,02% em 1999. CONCLUSÕES: Os conhecimentos da fisiopatologia, da senilidade e os avanços no manuseio do trauma cirúrgico estão permitindo estender os recursos da cirurgia cardíaca no grupo de paciente mais idoso. A escolhas da técnica anestésica deve ser criteriosa, bem como a hidratação, a assistência ventilatória e a analgesia pós-operatória, permitindo redução da morbimortalidade neste grupo de maior risco cirúrgico.JUSTIFICATIVA Y OBJETIVOS: El aumento de la expectativa de vida hace con que pacientes cada vez mas edosos tengan indicación de tratamiento quirúrgico de cardiopatias. Este estudio tiene como objetivo evaluar la incidencia de pacientes con más de 80 años sometidos a cirugía cardíaca en el Instituto del Corazón del Hospital de Clínicas de la FMUSP, en los últimos 16 años. MÉTODO: Fueron analizados, en el período de 1986 a 2001, el número de cirugías de revascularización del miocardio (RM y cirugía valvar (CV y, en cada grupo, el número de cirugías en pacientes con más de 80 a

  17. Protocolo de detección y tratamiento de la retinopatia del prematuro: Estudio retrospectivo y prospectivo entre los años 1995-2002.

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    Rodrigo Salcedo, Vicenta Maria

    2004-01-01

    RESUMEN El estudio se ha realizado con dos series de niños con retinopatía, una primera serie que se les detectó la enfermedad a 40 niños, y una segunda serie de 74 niños enfermos de ROP. Se crearon: 76 variables clínicas, 25 de estas variables eran maternas. 11 variables oftalmológicas. Después de analizados los resultados obtenidos y de acuerdo con los objetivos marcados, llegamos a la conclusión: 1) La incidencia de ROP en el hospital Universitario La Fe de Valencia: a...

  18. Carga inmediata de implantes monofásicos postextracción utilizando los expansores roscados atraumáticos: estudio retrospectivo 2001-2011

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    Riham Mostafa Eldibany

    2015-10-01

    Conclusiones: Tras haber analizado toda la secuencia referida a la carga inmediata, podemos concluir que los implantes monofásicos insertados con la aplicación de esta técnica son un procedimiento predecible: su éxito en el maxilar inferior en nuestro estudio de 10 años fue del 98%. Sin embargo, es necesario determinar los casos candidatos para dicho procedimiento, así como las características del implante que favorecen la implantación inmediata.

  19. Avaliação retrospectiva de artrodese cervical com enxerto autólogo versus hidroxiapatita Estudio retrospectivo de la artrodesis cervical con autoinjerto versus hidroxiapatita Retrospective study of cervical arthrodesis with autograft versus hydroxyapatite graft

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    Yoshinobu Nagasse

    2010-12-01

    Full Text Available OBJETIVO: os autores realizaram um estudo e compararam o resultado radiográfico no uso de hidroxiapatita e enxerto de crista ilíaca (autólogo no tratamento cirúrgico de hérnia discal cervical em um nível, sendo realizada artrodese cervical anterior com placa. MÉTODOS: foi realizado estudo retrospectivo com pacientes submetidos à artrodese cervical comparando-se dois grupos de dez pacientes: um em que foi utilizado enxerto de hidroxiapatita e outro em que foi utilizado enxerto de crista ilíaca (autólogo. Radiografias pós-operatórias foram mensuradas e comparadas, à busca de perdas de alinhamento angular. RESULTADOS: os dois tipos de enxerto demonstraram manter alinhamento em taxas similares, sendo observada consolidação óssea em todos os pacientes. O estudo não mostrou fragmentação do enxerto de hidroxiapatita ou soltura do material de síntese. CONCLUSÃO: nesta pequena série de casos não foi observada diferença significativa entre os resultados da artrodese cervical anterior com enxerto de hidroxiapatita em relação ao enxerto autólogo de ilíaco.OBJETIVOS: los autores realizaram un estudio y compararon el resultado radiográfico en el uso del hidroxiapatita y injerto de cresta ilíaca (autólogo, en el tratamiento quirúrgico de hernia discal cervical en un nivel, siendo realizada artrodesis cervical anterior con placa. MÉTODOS: fue realizado un estudio retrospectivo con pacientes, que habían sido sometidos a la artrodesis cervical con injerto de hidroxiapatita o injerto de cresta iliaca b.z autologa. Las radiografías postoperatorias habían sido mensuradas y comparadas, buscando para las pérdidas de alineación angular. RESULTADOS: los dos tipos de injerto habían demostrado manutención de alineación similares, donde la consolidación fue observada en todos los pacientes. El estudio no demostró la fragmentación del injerto de hidroxiapatita o de soltar el material de síntesis. CONCLUSIÓN: en esta peque

  20. Estudio retrospectivo de causas de trauma maxilofacial en Pasto, Colombia de 2001 a 2006 A retrospective study of maxillofacial trauma causes in Pasto, Colombia from 2001 to 2006

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    Ana Cristina Mafla

    2009-08-01

    Full Text Available Introducción: Las lesiones maxilofaciales son una condición frecuente en diferentes países, sin embargo, están asociadas a diversas causas. Metodología: Un estudio descriptivo fue realizado de Enero de 2001 a Diciembre de 2006 en tres hospitales y una institución de Pasto, Nariño, Colombia. 701 pacientes consecutivos del "Hospital San Pedro", "Hospital Universitario Departamental de Nariño", "Hospital Infantil Los Ángeles", y el Instituto de Medicina Legal y Ciencias Forenses Seccional Nariño - Putumayo fueron evaluados. Variables como año, género, distribución anatómica de la fractura, se incluyeron. Análisis descriptivos fueron usados para determinar porcentajes e intervalos de confianza. Resultados: Las causas más comunes fueron violencia, con 350 (49,9%, accidentes en motos con 104 (14,8%, en autos con 93 (13,3 %, y caídas con 66 (9,4%. Existió un incremento substancial de violencia en los años 2003 a 2004. Los niños de 0 a 6 años presentaron más caídas, mientras los jóvenes de 15 a 24 años se asociaron con violencia, al igual que accidentes en motos y automóviles. La violencia fue relacionada con fracturas de huesos propios de la nariz, caídas con lesiones naso-orbito-etmoidales, y accidentes en motos y automóviles con politraumatismo y fracturas panfaciales. Conclusiones: Debido a que la violencia, accidentes en motos y automóviles son las principales causas de lesiones maxilofaciales en la juventud, las políticas públicas deben ser dirigidas a ésta Salud UIS 2009; 41: 142-148Introduction: Maxillofacial injuries are a frequent condition in different countries; however, they are associated to different causes. Methodology: A descriptive study was performed from January 2001 to December 2006 at three hospitals and one institution from Pasto, Nariño, Colombia. 701 consecutive patients at "Hospital Los Angeles", "Hospital San Pedro", "Hospital Universitario Departamental de Nariño" and "Instituto de Medicina

  1. Estudio retrospectivo sobre la incidencia de las infecciones cérvico faciales en Hospital Pablo Arturo Suárez en el período comprendido entre enero del 2008 y diciembre del 2010

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    Santiago Javier Garcés Mora

    2015-12-01

    Full Text Available Las infecciones odontogénicas dentro del campo de la cirugía maxilofacial son muy frecuentes y con gran poder de diseminación a espacios faciales de la cabeza y del cuello (Raspall 2006. Por esta razón, el propósito de este estudio, es identificar el grupo poblacional de mayor afectación y determinar el espacio anatómico afectado más frecuente por estas entidades infecciosas.En este estudio retrospectivo se recolecta información de los pacientes atendidos en el período comprendido entre enero del 2008 y diciembre del 2010. Se evalúa: año, género, grupos etarios, patologías preexistentes y las infecciones odontogénicas con sus espacios anatómicos comprometidos, determinando frecuencias simples y conjuntas en función a los objetivos planteados.El crecimiento anual es del 25% en número de casos. De 650 casos, las mujeres presentan mayor prevalencia con el 59,4%. El grupo etario más afectado es el de 21 a 30 años. La diabetes es el antecedente patológico de base más común con 18 casos. Las infecciones localizadas representan el 73,5% de la muestra, mientras que el 26,5% evolucionaron a estadios infecciosos más complejos como las celulitis odontogénicas con el 15,8%. Los focos sépticos (raíces dentales abandonadas representan el 45,2% de las infecciones localizadas. Las celulitis afectan con más frecuencia el espacio geniano con el 48,5% mientras que los abscesos se desarrollan con más facilidad en el espacio submandibular con el 42,3%. La complicación infecciosa más común es la osteomielitis con 18 casos (2,8%. Las infecciones localizadas aumentan con la edad, mientras que los estadios celulíticos disminuyen con la edad, presentando mayor prevalencia en la niñez. Las mujeres en edad fértil (21 a 30 años es el grupo más vulnerable.

  2. Interação medicamentosa associada à reinternação hospitalar: estudo retrospectivo em um hospital geral Interacción medicamentosa asociada a la reinternación hospitalaria: estudio retrospectivo en un hospital general Hospital readmissions related to drug interactions: a retrospective study in a hospital setting

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    Cristiano Soares de Moura

    2012-12-01

    Full Text Available OBJETIVO: Analisar a relação entre interação medicamentosa potencial e reinternação hospitalar. MÉTODOS: Estudo retrospectivo com 1.487 pacientes maiores de 18 anos admitidos em um hospital geral em Vitória da Conquista, BA, de janeiro a dezembro de 2007. Os dados foram extraídos da Autorização de Internação Hospitalar do Sistema de Informação Hospitalar do Sistema Único de Saúde. O relacionamento probabilístico foi empregado para combinar múltiplas autorizações de uma mesma internação em um único registro e para identificar readmissões. Informações sobre prescrições foram agregadas manualmente aos registros do Sistema de Informação Hospitalar. Regressão logística foi utilizada para quantificar a influência de interação medicamentosa potencial e reinternação. Regressão de Cox foi empregada para testar a influência dessa variável no tempo até a primeira reinternação. RESULTADOS: Foram identificadas 99 readmissões (7% dos pacientes. Interação medicamentosa potencial foi encontrada em 35% das prescrições analisadas. Pacientes com potencial de interação medicamentosa na admissão prévia foram mais propensos à reinternação. A razão de chance ajustada indicou que esses pacientes tinham chance 2,4 vezes maior de readmissão; a taxa de risco ajustada mostrou que em pacientes com interação medicamentosa esse risco foi 79% maior (p OBJETIVO: Analizar la relación entre potencial interacción medicamentosa potencial y reinternación hospitalaria. MÉTODOS: Estudio retrospectivo con 1.487 pacientes mayores de 18 años admitidos en un hospital general en Vitória da Conquista, BA, Brasil, de enero a diciembre de 2007. Los datos fueron extraídos de la Autorización de Internación Hospitalaria del Sistema de Información Hospitalaria del Sistema Único de Salud Brasileño. La relación probabilística fue empleada para combinar múltiples autorizaciones de una misma internación en un único registro

  3. Associação entre glicemia de jejum e morbimortalidade perioperatória: estudo retrospectivo em pacientes idosos cirúrgicos Asociación entre glicemia de ayuno y morbimortalidad perioperatoria: estudio retrospectivo en pacientes ancianos quirúrgicos Association between fasting blood glucose levels and perioperative morbimortality: retrospective study in surgical elderly patients

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    Arthur Vitor Rosenti Segurado

    2007-12-01

    peri operatorias en la población de ancianos sometidos a procedimientos quirúrgicos todavía no se conocen. El objetivo de este estudio fue evaluar la Asociación entre glicemia de ayuno y morbimortalidad perioperatoria en pacientes quirúrgicos ancianos. MÉTODO: Se analizaron las hojas clínicas de pacientes de más de 60 años sometidos a diversos procedimientos quirúrgicos en un período de 6 meses, divididos de acuerdo con los valores de glicemia de ayuno en los grupos: 126 mg.dL-1. Fueron analizados en cuanto a la edad, estado físico (ASA, historial previo de diabetes melito (DM y tratamiento y riesgo cardíaco perioperatorio cirugía específica. A través de análisis univariada y de un modelo de regresión logística multivariada, se evaluó la relación entre los desenlaces (frecuencia de complicaciones postoperatorias (CPO y óbitos y las variables: glicemia de ayuno, historial previo de DM, estado físico (ASA y riesgo cardíaco. RESULTADOS: Hubo asociación estadística apenas entre los grupos glicémicos y las variables estado físico e historial previo de DM. Todas las variables estudiadas revelaron asociación estadística con relación a la mayor frecuencia de CPO y óbitos, excepto la variable presencia de historial previo de DM que no presentó relación con óbitos. En el modelo de regresión logística multivariada, hubo asociación entre las variables riesgo cardíaco y glicemia en función de la incidencia de CPO, mientras apenas las variables estado físico y riesgo cardíaco revelaron asociación estadística en función de los óbitos. CONCLUSIONES: Ese estudio retrospectivo mostró que, para la población pacientes ancianos estudiada, hubo asociación significativa entre glicemias por encima de 100 mg.dL-1 y morbimortalidad perioperatoria.BACKGROUND AND OBJECTIVES: The relationship between altered blood glucose levels and perioperative complications in elderly patients undergoing surgeries are not known. The objective of this study was to

  4. Experiência clínica com o uso de sedativos em terapia intensiva: estudo retrospectivo Experiencia clínica con el uso de sedativos en la terapia intensiva: estudio retrospectivo Clinical experience with sedatives in the intensive care unit: a retrospective study

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    Geraldo Rolim Rodrigues Júnior

    2002-11-01

    utilizada para facilitar a ventilação artificial e tratar os problemas de natureza psiquiátrica. Fentanil, isoladamente ou em associação com midazolam, foi o agente mais utilizado.JUSTIFICATIVA Y OBJETIVOS: Entre las indicaciones más frecuentes de sedación en pacientes internados en Unidades de Terapia Intensiva (UTI están la institución y la manutención de ventilación artificial, la ansiedad y procedimientos desconfortables o dolorosos. El objetivo de este estudio retrospectivo fue verificar las indicaciones y las técnicas más comunes de sedación en pacientes graves internados en la Unidad de Terapia Intensiva Quirúrgica de la Escuela Paulista de Medicina (EPM/UNIFESP durante un período de 11 meses. MÉTODO: Después de haber sido excluidos los pacientes que permanecieron en la UTI menos de 24 horas o estaban sin exámenes indispensables para el cálculo del índice de gravedad (APACHE II, la muestra quedó reducida a 307 pacientes. Fueron analizadas las técnicas más utilizadas, las indicaciones de sedación y la asociación de bloqueadores neuromusculares. RESULTADOS: La sedación fue administrada en 37,4% de los pacientes. Entre las indicaciones de sedación están los disturbios de naturaleza psiquiátrica, como delirio, agitación, miedo y ansiedad. Éstas correspondieron a 25,77% de todas las indicaciones. La mayoría de los pacientes ventilados artificialmente también necesita de sedativos. Instalación y manutención de ventilación mecánica correspondieron a la mayoría de las indicaciones, alrededor de 57,73% de los pacientes sedados. Procedimientos como intubación traqueal y broncoscopia tuvieron 11,34% de las indicaciones y control del metabolismo (coma barbitúrico y tétano, 5,15%. Las técnicas mas comúnmente utilizadas incluyeron opioides aislados o asociados a benzodiazepínicos. En este estudio, el fentanil fue utilizado en 58% de las técnicas, aisladamente, y en 21,64% asociado al midazolam. Haloperidol, diazepam, propofol y

  5. Disturbios da olfacao: estudo retrospectivo

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    Luciano Lobato Gregorio

    2014-01-01

    Full Text Available Introdução: O olfato, fenômeno subjetivo de grande importância, é pouco compreendido e estudado no ser humano. Médicos com maior conhecimento sobre os distúrbios desse sentido tendem a considerar a doença mais importante e manejar melhor o diagnóstico e o tratamento. Objetivo: Descrever a amostra dos pacientes com queixa principal de distúrbios do olfato e mostrar a experiência do serviço no manejo e tratamento. Delineamento: Estudo retrospectivo de coorte histórica com corte transversal. Materiais e métodos: Descrição da amostra e avaliação de resposta ao tratamento de pacientes com queixa principal de hiposmia ou anosmia atendidos no ambulatório de Rinologia no período de janeiro de 2005 a outubro de 2011. Resultados: Dos 38 pacientes com distúrbio da olfação, 68,4% dos pacientes apresentaram queixa de hiposmia e 31,5% de anosmia, com duração média de 30,8 meses. Os diagnósticos etiológicos principais foram idiopática (31,5%, rinopatia alérgica (28,9% e RSC com pólipos (10,5%. As respostas ao tratamento com corticosteroide tópico e ácido alfa-lipoico foram variáveis, assim como na literatura. Conclusão: Maior importância deve ser dada aos distúrbios do olfato na prática do otorrinolaringologista, uma vez que o diagnóstico diferencial é amplo e pode trazer grande morbidade ao paciente, com impacto na sua qualidade de vida.

  6. A retrospective study of pediatric endoscopy as performed in an adult endoscopy unit Estudio retrospectivo sobre la endoscopia pediátrica desarrollada en un servicio de endoscopias de adultos

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    L. Julián-Gómez

    2010-02-01

    Full Text Available Gastrointestinal endoscopy is a safe, efficient technique with minimal complications, and a useful diagnostic tool for the pediatric population. Under ideal conditions endoscopies for children should be performed by experienced pediatric endoscopists. In this study we report our experience with pediatric endoscopy at the general adult endoscopy unit in our hospital. Our goal is to quantify the number of endoscopies performed in children, as well as their indications and findings, the type of sedation or anesthesia used, and the time waiting for the test to occur. Our experience demonstrates that endoscopists in a general adult gastroenterology department, working together with pediatricians, may perform a relevant number of endoscopies in children in a fast, safe, effective manner.La endoscopia gastrointestinal es una técnica segura y eficiente con mínimas complicaciones, así como una útil herramienta diagnóstica en la población pediátrica. En condiciones ideales, las endoscopias en niños deberían ser realizadas por endoscopistas pediátricos experimentados. En este estudio reportamos nuestra experiencia en la realización de endoscopias pediátricas en la Unidad de Endoscopias general de adultos de nuestro hospital. El objetivo es cuantificar la cantidad de endoscopias realizadas en niños, así como las indicaciones y hallazgos de las mismas, el tipo de sedación o anestesia empleado y el tiempo de espera para la realización de la prueba. Nuestra experiencia demuestra que los endoscopistas de un servicio de gastroenterología general de adultos, en colaboración con pediatras, pueden realizar un número importante de endoscopias a niños, de forma rápida, segura y eficaz.

  7. Uso de dexmedetomidina em pacientes obesos mórbidos submetidos a gastroplastia: estabilidade cardiovascular e consumo de anestésicos venosos. Estudo retrospectivo Uso de dexmedetomidina en pacientes obesos mórbidos sometidos a gastroplastia: estabilidad cardiovascular y consumo de anestésicos venosos. Estudio retrospectivo Dexmedetomidine in morbid obese patients undergoing gastroplasty: cardiovascular stability and consumption of intravenous anesthetics. A retrospective study

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    Luiz Piccinini Filho

    2006-04-01

    o houve efeitos colaterais imputáveis ao uso da dexmedetomidina.JUSTIFICATIVA Y OBJETIVOS: La utilización de agentes anestésicos potentes y de corta duración es fundamental en pacientes sometidos a la intervención quirúrgica bariátrica. La dexmedetomidina, agonista alfa 2-adrenérgica, surgió como una opción de auxilio a la técnica de anestesia venosa. El objetivo de esta investigación fue la de evaluar la eficacia de la dexmedetomidina asociada a la anestesia venosa en pacientes obesos mórbidos, sometidos a la gastroplastia. MÉTODO: Análisis retrospectivo de pacientes portadores de obesidad mórbida, sometidos a la intervención quirúrgica bariátrica abierta, bajo anestesia con propofol y alfentanil con o sin dexmedetomidina. Los pacientes fueron colocados en dos grupos: Control (propofol y alfentanil y Dexmedetomidina (propofol, alfentanil y dexmedetomidina. El mantenimiento de la anestesia en los dos grupos constó de: propofol = 0,075 a 0,1 mg.kg-1.min-1 y alfentanil = 0,75 a 1 µg.kg-1.min-1; en el grupo Dexmedetomidina en la dosis inicial de 1 µg.kg-1 en 10 min y mantenimiento con 0,4 a 0,7 µg.kg-1.h-1. Las variables estudiadas fueron la edad, sexo, IMC, tiempo quirúrgico y de despertar, frecuencia cardiaca (FC, presión arterial sistólica y diastólica (PAS, PAD, saturación periférica de hemoglobina (SpO2, consumo de propofol y alfentanil y efectos colaterales. RESULTADOS: Se registró una reducción significativa en el consumo de propofol y alfentanil en el grupo Dex-medetomidina. La FC presentó variación significativa apenas en el grupo Dexmedetomidina. La PAS y la PAD presentaron una reducción estadística significativa en los dos grupos en los primeros 20 min, estabilizándose a continuación. Los pacientes de los dos grupos no presentaron efectos colaterales. CONCLUSIONES: Ese estudio demostró la eficacia del uso de la dexmedetomidina asociada a la anestesia venosa con propofol y alfentanil, trayendo una reducción del consumo de los

  8. Derivaciones al Servicio de Urgencias del hospital en una población de ancianos residentes: Estudio retrospectivo sobre sus causas y adecuación Hospital transfers from a population of elderly residents: A retrospective study about the causes and suitability

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    José Carlos Bermejo Higuera

    2010-09-01

    Full Text Available Objetivo: analizar las causas y la adecuación de las derivaciones de ancianos institucionalizados al Servicio de Urgencias del hospital. Método: estudio descriptivo retrospectivo transversal sobre la población de una residencia de la Comunidad de Madrid. Se recogieron datos de 45 pacientes derivados durante el año 2008, con un total de 62 derivaciones. Derivación adecuada o pertinente fue aquella que cumpliera uno de los siguientes criterios: 1 el paciente ingresó o estuvo en observación más de 24 horas; 2 precisó ser valorado por un especialista y/o requirió pruebas diagnósticas no disponibles en el centro; y 3 necesitó tratamiento no disponible en el centro. Análisis estadístico descriptivo. Resultados: el 98,4% de las derivaciones cumplió los criterios de adecuación; 67% Criterio 1,21% Criterio 2 y no otros, y 77,4% Criterio 3. La causa más frecuente de derivación fue la sospecha de fractura poscaída (32,3%. El porcentaje anual de fallecidos (22,38% fue menor que el observado en otras residencias madrileñas, de ellos, el 15,55% falleció en el hospital.Aim: to analyse the causes and suitability of elderly resident transfers to hospital emergencies service. Methods: a retrospective and descriptive study about the resident population in a Residence of Comunidad de Madrid. We recorded data from 45 patients transferred in 2008, out of a total of 62 transfers. A suitable or appropriate derivation was one fulfilling at least one of the following criteria: 1-the patient was admitted to hospital or stayed in observation for more than 24 hours, 2- the patient had to be seen by a specialist or required a diagnosis test that was not available in the centre, 3- the patient needed treatment that was not available in the centre. The statistical analysis was descriptive. Results: 98.4% of the transfers complied with the suitability criteria: 67% criterion 1,21% criterion 2 but not other and 77% criterion 3. The most frequent cause for

  9. Miocardiopatía diabética: un punto de vista retrospectivo

    OpenAIRE

    Rafael Ramírez; Montserrat Durán; Javier Márquez

    2018-01-01

    Objetivo: Estimar la prevalencia de pacientes con probable miocardiopatía diabética (sin exigir biopsia endomiocárdica), analizando sus características y comparándolas con pacientes no diabéticos con insuficiencia cardiaca idiopática. Métodos: Estudio retrospectivo sobre una cohorte de 270 pacientes que ingresaron de manera consecutiva por insuficiencia cardiaca. De estos se excluyeron del estudio todos aquellos que tuvieran una causa conocida de insuficiencia cardiaca (cardiopatía isquémi...

  10. Estudio clínico retrospectivo del uso de un sistema de hidrocirugía en pacientes lesionados medulares con úlceras por presión crónicas Retrospective clinical study of an hydrogurgery system on spinal cord injured patients with chronic pressure ulcers

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    J.M. Arévalo Velasco

    2011-03-01

    Full Text Available Realizamos un estudio clínico retrospectivo con pacientes lesionados medulares crónicos en el Hospital Nacional de Parapléjicos (Toledo, España, intervenidos quirúrgicamente por una o varias úlceras por presión de carácter crónico durante el año 2008. Revisamos 84 historias clínicas de pacientes a los cuales se realizaron 141 procedimientos quirúrgicos. Sólo en 8 casos se realizó una cirugía puramente de limpieza (bisturí más hidrocirugía sin realizar consecutivamente el tratamiento de cobertura de la lesión. Los restantes 133 procedimientos de limpieza más cobertura inmediata se distribuyeron en 2 grupos según el tipo de desbridamiento realizado: grupo I (n = 71, sólo desbridamiento quirúrgico con bisturí y grupo II (n = 62 desbridamiento con bisturí más uso posterior de un sistema de hidrocirugía de flujo continuo a alta presión. Según la localización, las lesiones ulcerosas tratadas fueron: isquiáticas 69 (48,94 %, sacras 49 (34,75 %, trocantéreas 15 (10,63 % y otras (talones y maléolos 8 (5,67%. Como conclusiones, establecemos que más del 54 % de los procedimientos llevados a cabo (72 de 133 curaron en la primera intervención y no necesitaron más cirugías; un 38% (51 de 133 fueron intervenciones realizadas en pacientes con úlceras muy evolucionadas y/o de difícil solución; la tasa de recidivas al año fue del 4,4 %; no encontramos diferencias significativas en cuanto a la tasa de curación entre los grupos I y II (p We carried out a retrospective study on spinal cord injured patients from the National Hospital for Paraplegics (Toledo, Spain, who were surgically treated during 2008 to alleviate the problems elicited by one or more pressure ulcers of chronic nature. We reviewed the clinical histories of 84 patients that received 141 surgical procedures, 8 were of radical nature (scalpel plus hidrosurgery without wound covering. The remaining 133 procedures of surgical cleaning and immediate wound

  11. Utilización de los grupos clínicos ajustados en un centro de atención primaria español: estudio retrospectivo de base poblacional Adjusted clinical groups use at a Spanish primary care center: a retrospective, population-based study

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    Antoni Sicras-Mainar

    2010-01-01

    Full Text Available OBJETIVOS: Evaluar los resultados de la aplicación del sistema de clasificación mediante grupos clínicos ajustados (GCA en un centro de atención primaria de salud (APS de una población española. MÉTODOS: Estudio transversal retrospectivo a partir de los registros médicos informatizados de los pacientes atendidos ambulatoriamente durante 2007 en el centro de salud La Roca, administrado por una empresa de gestión de servicios de salud en La Roca del Vallès, Barcelona, España. Los GCA se conformaron según la Clasificación Internacional de Enfermedades, 9.ª revisión, modificación clínica. Se calcularon los pesos relativos medios en dólares estadounidenses de cada GCA respecto al costo medio total y, a partir de ellos, se crearon las bandas de utilización de recursos. Se determinaron los índices de riesgo (IR y eficiencia (IE con respecto a 2006 y se estimó el poder explicativo de la clasificación empleada. RESULTADOS: Se estudiaron 8 294 pacientes, para una cobertura de 82,7%, con una media de 4,1 episodios por paciente, 6,9 visitas por paciente y 5,7 visitas por habitante al año. A siete GCA correspondió 51,0% de los pacientes atendidos. El IR fue de 1,015, el IE en las visitas de 0,975 y el poder explicativo de la clasificación en GCA fue de 53,4% para las visitas y de 74,8% para los episodios. CONCLUSIONES: El sistema de GCA permitió agrupar a los pacientes de una población según su estado clínico y puede ayudar, entre otros aspectos, en la asignación de recursos y la evaluación de la eficiencia de los equipos de APS.OBJECTIVES: To evaluate the results of implementing a classification system based on adjusted clinical groups (ACG at a primary health care (PHC in a Spanish population. METHODS: A retrospective, cross-sectional study based on the computerized medical records of outpatients seen in 2007 by the La Roca clinic, administered by a health services management company in La Roca del Vallès, Barcelona, Spain

  12. Coronal magnetometry

    CERN Document Server

    Zhang, Jie; Bastian, Timothy

    2014-01-01

    This volume is a collection of research articles on the subject of the solar corona, and particularly, coronal magnetism. The book was motivated by the Workshop on Coronal Magnetism: Connecting Models to Data and the Corona to the Earth, which was held 21 - 23 May 2012 in Boulder, Colorado, USA. This workshop was attended by approximately 60 researchers. Articles from this meeting are contained in this topical issue, but the topical issue also contains contributions from researchers not present at the workshop. This volume is aimed at researchers and graduate students active in solar physics. Originally published in Solar Physics, Vol. 288, Issue 2, 2013 and Vol. 289, Issue 8, 2014.

  13. Comparação entre raquianestesia, bloqueio combinado raqui-peridural e raquianestesia contínua para cirurgias de quadril em pacientes idosos: estudo retrospectivo Comparación entre raquianestesia, bloqueo combinado raqui-peridural y raquianestesia continua para cirugías de cuadril en pacientes ancianos: estudio retrospectivo Comparison between spinal, combined spinal-epidural and continuous spinal anesthesias for hip surgeries in elderly patients: a retrospective study

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    Luiz Eduardo Imbelloni

    2002-06-01

    Full Text Available JUSTIFICATIVA E OBJETIVOS: Diversas questões envolvem os estudos, as análises e o tamanho da amostra para que sejam demonstrados os benefícios da anestesia regional. Análise de dados geralmente custa menos e requer menos tempo quando comparado com amplo estudo aleatório controlado. Esta análise retrospectiva compara a raquianestesia contínua, o bloqueio combinado raqui-peridural e a raquianestesia simples para cirurgias de quadril em pacientes idosos durante quatro anos, para determinar as possíveis vantagens e desvantagens das três técnicas. MÉTODO: Foram avaliados 300 prontuários sendo que: 100 pacientes receberam raquianestesia simples (Grupo 1, 100 receberam bloqueio combinado raqui-peridural (Grupo 2 e 100 receberam raquianestesia contínua (Grupo 3 nos últimos quatro anos. Todos os bloqueios foram realizados em decúbito lateral esquerdo. Foram avaliados: sucesso de punção, nível da analgesia, bloqueio motor de membros inferiores, qualidade da anestesia, necessidade de complementação, incidência de falhas, parestesias, cefaléia pós-punção, alterações cardiovasculares, confusão mental e delírio, transfusão sangüínea e mortalidade. RESULTADOS: Não existiu diferença significativa entre os grupos em relação a idade, peso e sexo. Os pacientes do grupo 2 foram menores do que os do grupo 1 e 3. As doses utilizadas foram de 15,30 mg de bupivacaína no grupo 1; 23,68 mg no grupo 2 e 10,10 mg no grupo 3. Não foi encontrada diferença significativa (p JUSTIFICATIVA Y OBJETIVOS: Diversas cuestiones envuelven los estudios, las análisis y el tamaño de la muestra para que sean demostrados los beneficios de la anestesia regional. Las análisis de datos generalmente cuestan menos y requieren menos tiempo, cuando comparado con un amplio estudio aleatorio controlado. Esta análisis retrospectiva compara la raquianestesia continua, el bloqueo combinado raqui-peridural y la raquianestesia simple para cirugías de cuadril en

  14. Estudo retrospectivo das infecções pós-operatórias em cirurgia de coluna: correlação com o número de limpezas cirúrgicas realizadas Estudio retrospectivo de infecciones postoperatorias en cirugía de espina dorsal: correlación con el número de desbridamientos quirúrgicos realizados Retrospective study of post-operative infections in spine surgery: correlation with the number of surgical debridement performed

    Directory of Open Access Journals (Sweden)

    Guilherme Pereira Corrêa Meyer

    2011-01-01

    ón primaria de la espina dorsal (osteomielitis o espondilodiscitis totalizando 3 casos. Variables relativas al paciente, realización de tratamientos y resultados fueron evaluadas y correlacionadas con las variables clave: número de desbridamientos quirúrgicos y cultivos aislados de agentes infecciosos. RESULTADOS: La tasa de infección, después de la cirugía, fue 9,83%. Algunas variables fueron relacionadas con el número de desbridamientos quirúrgicos realizados y no fue posible establecer alguna relación. No obstante, se descubrió que pacientes con un mayor número de tratamientos quirúrgicos realizados tuvieron una tasa mayor de dolor postoperatorio. CONCLUSIÓN: Pacientes que recibieron un mayor número de tratamientos realizados tuvieron más dolor en el período postoperatorio. No hubo correlación, estadísticamente significativa, entre el número de desbridamientos o agentes infecciosos, o con otras variables. Puede ser necesario tener un mayor número de pacientes en el estudio, a fin de identificar otras relaciones.OBJECTIVE: To evaluate the characteristics of post-operative infections and determine their resolution in relation to the number of surgical debridement and infectious agents. METHOD: We collected all records of patients who developed post-operative infection for 30 months and several variables were analyzed and correlated. In those 30 months, 40 patients developed post-operative infection of a total of 410 surgeries. We excluded cases of primary infection of the spine (osteomyelitis or spondylodiscitis totaling 3 cases. Variables related to the patient, procedure and outcome were evaluated and correlated with the key variables: number of surgical debridement and infectious agents isolated from cultures. RESULTS: The rate of infection after surgery was 9.83%. Several variables were related to the number of surgical debridement performed and it was not possible to establish any relationship. However, it was found that patients with higher number

  15. Asociación del anticuerpo anti-C1q con las manifestaciones clínicas, hematológicas e inmunológicas en el Lupus Eritematoso Sistémico : Estudio observacional retrospectivo de 135 casos.

    OpenAIRE

    Córica, María Emilia

    2012-01-01

    : Las concentraciones de anticuerpo anti-C1q están elevadas en los pacientes afectados de LES. Según algunos estudios la presencia de este anticuerpo está asociada a la nefropatía lúpica, sin embargo en otros estudios esta relación no se comprobó. En nuestro trabajo relacionamos la positividad del anticuerpo anti-C1q con las manifestaciones clínicas, hematológicas e inmunológicas de la enfermedad. A diferencia de estudios previos sólo pudimos establecer una relación estadísticamente significa...

  16. Roll of the adjuvant radiotherapy. Kidney cancer. Stage III. Results to 5 years. Observational, descriptive, retrospective, quantitative and comparative study with data numerical description; Rol de la radioterapia adyuvante. Cancer de rinion. Estadio III. Resultados a 5 anios. Estudio observacional, descriptivo, retrospectivo, cuantitativo y comparativo, con descripcion numerica de los datos

    Energy Technology Data Exchange (ETDEWEB)

    Lione, M; Tissera, N; Mandachain, M [Centro de Oncologia y Terapia Radiante, Santa Rosa, La Pampa (Argentina)

    2007-07-01

    Kidney cancer represents 3 % of the tumors in adults. In the United States, the 45% is diagnosed in early stages. Its natural history is characterized for being absolutely unpredictable and probably related to hormonal, immunologic and unknown factors. There are patients in advanced stage with prolonged or low average survival and even with metastasis declination. These particularities along with the lack of prospective random studies make difficult to establish which is the roll of the adjuvant radiotherapy, being considered not standard since 1997. [Spanish] El cancer de rinion representa el 3% de los tumores en adultos. En Estados Unidos el 45% se diagnostica en estadios tempranos. Su historia natural se caracteriza por ser absolutamente impredecible, probablemente relacionado a factores hormonales, inmunologicos y desconocidos; hay pacientes con enfermedad avanzada con prolongada o corta supervivencia media e incluso con regresion de metastasis. Estas particularidades, juntamente con la falta de estudios prospectivos aleatorios dificultan establecer cual es el rol de la radioterapia adyuvante, considerandose no estandar desde 1997.

  17. Metástasis cervical contralateral en el carcinoma epidermoide de la cavidad oral: Estudio clínico analítico retrospectivo en 315 pacientes primariamente tratados con cirugía Contralateral neck metastasis in squamous cell carcinoma of the oral cavity: An analytical retrospective clinical study of 315 patients primarily treated with surgery

    Directory of Open Access Journals (Sweden)

    R. González-García

    2008-06-01

    Full Text Available Objetivos. Existen en la literatura numerosos estudios en relación con los factores pronósticos implicados en la aparición de metástasis cervicales ipsilaterales en el carcinoma epidermoide de cavidad oral. Sin embargo, no existen estudios clínicos amplios acerca de la asociación de factores clínico-patológicos y la aparición de metástasis cervicales contralaterales tras la resección quirúrgica del tumor primario. El propósito de este estudio es el análisis de los factores implicados en la aparición de metástasis cervical contralateral en pacientes con carcinoma epidermoide de cavidad oral primariamente tratados con cirugía. Pacientes y métodos. Se analizó una serie de 315 pacientes consecutivos con carcinoma epidermoide de la cavidad oral no tratados previamente. Se realizó un estudio complementario del subgrupo de 203 pacientes con carcinoma epidermoide del borde lateral de la lengua libre, por tratarse de un grupo muy prevalente en la serie analizada. Todos los pacientes recibieron tratamiento quirúrgico con o sin tratamiento radioterápico adyuvante. Varias fueron las variables clínicas e histopatológicas analizadas, como son: las características clínicas del tumor, el estadio tumoral, el grado de diferenciación histológica, el tipo de disección cervical, la supervivencia enfermedad- específica, los márgenes quirúrgicos en la pieza resecada, la extensión ganglionar extracapsular, la diseminación perineural y la afectación ósea. Resultados. La duración media del seguimiento de los pacientes que sobrevivieron fue de 70,9 ± 49,6 meses. Ochenta y tres pacientes murieron a causa de la enfermedad a lo largo del seguimiento. Cuarenta y siete de estos pertenecían al subgrupo de pacientes con carcinoma epidermoide de lengua. Un total de 147 pacientes permanecía vivo sin evidencias de recurrencia de la enfermedad al final del periodo de seguimiento, 116 de los cuales correspondían al subgrupo de pacientes con

  18. Formation of coronal cavities

    International Nuclear Information System (INIS)

    An, C.H.; Suess, S.T.; Tandberg-Hanssen, E.; Steinolfson, R.S.

    1986-01-01

    A theoretical study of the formation of a coronal cavity and its relation to a quiescent prominence is presented. It is argued that the formation of a cavity is initiated by the condensation of plasma which is trapped by the coronal magnetic field in a closed streamer and which then flows down to the chromosphere along the field lines due to lack of stable magnetic support against gravity. The existence of a coronal cavity depends on the coronal magnetic field strength; with low strength, the plasma density is not high enough for condensation to occur. Furthermore, we suggest that prominence and cavity material is supplied from the chromospheric level. Whether a coronal cavity and a prominence coexist depends on the magnetic field configuration; a prominence requires stable magnetic support

  19. Can coronal hole spicules reach coronal temperatures?

    Science.gov (United States)

    Madjarska, M. S.; Vanninathan, K.; Doyle, J. G.

    2011-08-01

    Aims: The present study aims to provide observational evidence of whether coronal hole spicules reach coronal temperatures. Methods: We combine multi-instrument co-observations obtained with the SUMER/SoHO and with the EIS/SOT/XRT/Hinode. Results: The analysed three large spicules were found to be comprised of numerous thin spicules that rise, rotate, and descend simultaneously forming a bush-like feature. Their rotation resembles the untwisting of a large flux rope. They show velocities ranging from 50 to 250 kms-1. We clearly associated the red- and blue-shifted emissions in transition region lines not only with rotating but also with rising and descending plasmas. Our main result is that these spicules although very large and dynamic, are not present in the spectral lines formed at temperatures above 300 000 K. Conclusions: In this paper we present the analysis of three Ca ii H large spicules that are composed of numerous dynamic thin spicules but appear as macrospicules in lower resolution EUV images. We found no coronal counterpart of these and smaller spicules. We believe that the identification of phenomena that have very different origins as macrospicules is due to the interpretation of the transition region emission, and especially the He ii emission, wherein both chromospheric large spicules and coronal X-ray jets are present. We suggest that the recent observation of spicules in the coronal AIA/SDO 171 Å and 211 Å channels probably comes from the existence of transition region emission there. Movie is available in electronic form at http://www.aanda.org

  20. Prevalencia de Candidiasis Bucal en pacientes VIH/SIDA: Estudio retrospectivo

    OpenAIRE

    Tovar, V; Albornoz, E; Guerra, M; Lazarde, J

    2004-01-01

    El objetivo de este trabajo fue conocer la prevalencia de Candidiasis Bucal en un grupo de pacientes VIH/SIDA que acudieron al Servicio de Atención a Pacientes con Enfermedades Infectocontagiosas (SAPEI) de la Facultad de Odontología de la UCV. Se estudiaron 509 pacientes de los cuales 151 pacientes al examen clínico presentaron lesiones bucales de Candidiasis, de estos, 119 eran hombres y 32 mujeres, con un rango de edades entre 19 y 64 años y un promedio de 38,12 años. Los pacientes fueron ...

  1. MEJORAS DE ACCESIBILIDAD VIARIA: UN ESTUDIO RETROSPECTIVO PARA LA ESPAÑA PENINSULAR

    Directory of Open Access Journals (Sweden)

    Adelheid Holl

    2011-01-01

    Full Text Available Desde los años ochenta, se ha incrementado considerablemente la red de autovías y autopistas en España. Esta investigación presenta un análisis de las mejoras en accesibilidad que los programas de construcción de vías rápidas de gran capacidad han generado. Se calculan dos indicadores de accesibilidad a nivel municipal para toda la península española y para el periodo de 1980-2005: acceso a autovías y autopistas interregionales y potencial de mercado. La distancia media de los municipios a la autovía o autopista mas cercana se ha reducido considerablemente. En general, la accesibilidad ha mejorado en todo el país, pero no todas las zonas se han beneficiado al mismo nivel.

  2. Cáncer de Tiroides: Estudio descriptivo retrospectivo Thyroid carcinoma: A descriptive retrospective study

    Directory of Open Access Journals (Sweden)

    Carolina C. González

    2006-12-01

    Full Text Available Entre todos los tumores, el carcinoma tiroideo (CT es poco frecuente, se caracteriza por su lenta evolución y elevado porcentaje de curación. Nuestro objetivo es estudiar las características de los pacientes con CT. Analizamos retrospectivamente a 171 pacientes, edad media al diagnóstico 41.1( ± 14.6 años, que consultaron entre los años 2000-04 por CT. Se evaluaron datos de anamnesis, métodos de diagnóstico, anatomía patológica y evolución. Agrupamos a los tumores por el tamaño y según TNM (tumor-adenopatía-metástasis en estadios (E. La presencia de tiroglobulina estimulada (Tg > 2 ng/ml e imagen positiva (con 131I u otro radiotrazador fueron consideradas como positivas para CT residual. De la población total el 88% fue sexo femenino, el 62% menores de 45 años, y el 77.1% tuvo función tiroidea normal. La punción con aguja fina (PAAF fue diagnóstica en 78%. El 96% fue carcinoma papilar (CTP, 63% presentaban E I; 14% E II; 19% E III y 4% E IV. Se detectó CT residual en el 90% de los pacientes con Tg entre 2 y 10, y en el 100% con Tg > 10 ng/ml, mientras que con Tg The thyroid carcinoma (TC is not very frequent among all cancers. Its course is slow and is high potentially curable. Our aim was to analyse the characteristics in patients with TC. A retrospective analysis on 171 patients, with an average age of 41.1 (±14,6, who asked for TC to our service between the years 2000-04, was performed. From case histories it was evaluated: anamnesis, diagnostic image, histopathology and evolution. Tumours were grouped for size and TNM (tumour-nodule-metastasis in stages (S. A stimulated serum thyroglobulin level > 2 ng/ml and positive image with 131I or another nuclear marker were considered as positive for residual TC. In the totality of the analyzed patients 88% were female, 62% below 45 years old, and in 77% the thyroid function was normal. The fine needle aspiration (FNA was diagnostic in 78%. Papillary thyroid carcinoma (PTC in 96%. The 63% was SI; 14% SII; 19% SIII and 4% SIV. During follow-up, we observed that 90% of patients with Tg between 2 and 10 had evidence of residual TC, and 100% with Tg > 10 ng/ml, whereas 18% of those whose stimulated Tg < 2 presented positive image. There was not found significative correlation with pathologic antecedents or relevant image signs. In conclusion: TCP was the most frequent carcinoma in women, in patients younger than 45 years and in those who have euthyroid function. A stimulated serum thyroglobulin level was a good indicator for residual TC, but failed to select those patients who were disease free.

  3. Coronal Waves and Oscillations

    Directory of Open Access Journals (Sweden)

    Nakariakov Valery M.

    2005-07-01

    Full Text Available Wave and oscillatory activity of the solar corona is confidently observed with modern imaging and spectral instruments in the visible light, EUV, X-ray and radio bands, and interpreted in terms of magnetohydrodynamic (MHD wave theory. The review reflects the current trends in the observational study of coronal waves and oscillations (standing kink, sausage and longitudinal modes, propagating slow waves and fast wave trains, the search for torsional waves, theoretical modelling of interaction of MHD waves with plasma structures, and implementation of the theoretical results for the mode identification. Also the use of MHD waves for remote diagnostics of coronal plasma - MHD coronal seismology - is discussed and the applicability of this method for the estimation of coronal magnetic field, transport coefficients, fine structuring and heating function is demonstrated.

  4. Toxoplasmose em primatas neotropicais: estudo retrospectivo de sete casos

    Directory of Open Access Journals (Sweden)

    Renata A. Casagrande

    2013-01-01

    Full Text Available A toxoplasmose é considerada uma doença parasitária fatal em primatas neotropicais. O objetivo deste trabalho foi descrever, através de um estudo retrospectivo, os casos de toxoplasmose em primatas neotropicais. No período de 1999-2009 foram realizados 86 exames anatomopatológicos em primatas e a toxoplasmose foi a enfermidade mais comum (7/86, relatando-se um caso em sagui-do-tufo-preto (Callithrix penicillata e seis em bugio-ruivo (Alouatta guariba. Dois animais foram encontrados mortos e cinco morreram em poucos dias. Os sinais clínicos mais frequentes foram apatia e anorexia (5/7, distensão abdominal (4/7 e febre (3/7. Na necropsia observou-se esplenomegalia (4/7, hemorragia do trato digestório, linfonodos e bexiga (4/7, pulmões avermelhados (3/7 e hepatomegalia (2/7. No exame histopatológico evidenciou-se hepatite (7/7, esplenite (3/7, miocardite (2/7, enterite (2/7, linfadenite (1/7 e sialite (1/7 necróticas e, pneumonia intersticial (4/7. Em fígado, pulmões, baço, coração, linfonodos e glândula salivar havia taquizoítos de Toxoplasma gondii que foram também detectados pelo exame de imuno-histoquímica anti-T. gondii em fígado, baço e pulmões (5/7. A toxoplasmose pode causar alta mortalidade em colônias de primatas neotropicais e representar mais uma ameaça à conversação dessas espécies em cativeiro. Sendo assim, medidas preventivas devem ser tomadas para evitar a contaminação desses animais.

  5. Coronal mass ejections and coronal structures

    International Nuclear Information System (INIS)

    Hildner, E.; Bassi, J.; Bougeret, J.L.

    1986-01-01

    Research on coronal mass ejections (CMF) took a variety of forms, both observational and theoretical. On the observational side there were: case studies of individual events, in which it was attempted to provide the most complete descriptions possible, using correlative observations in diverse wavelengths; statistical studies of the properties of CMEs and their associated activity; observations which may tell us about the initiation of mass ejections; interplanetary observations of associated shocks and energetic particles; observations of CMEs traversing interplanetary space; and the beautiful synoptic charts which show to what degree mass ejections affect the background corona and how rapidly (if at all) the corona recovers its pre-disturbance form. These efforts are described in capsule form with an emphasis on presenting pictures, graphs, and tables so that the reader can form a personal appreciation of the work and its results

  6. Otomycosis: a retrospective study Otomicoses: um estudo retrospectivo

    Directory of Open Access Journals (Sweden)

    Zélia Braz Vieira da Silva Pontes

    2009-06-01

    Full Text Available Otomycosis is a fungal infection of the external ear canal with only a few studies about its real frequence in Brazil. AIM: to evaluate otomycosis frequence and characteristics in patients with clinical suspicion of external otitis. STUDY DESIGN: Retrospective study with transversal cohort (2000-2006. MATERIALS AND METHODS:103 patients were assigned to mycological diagnosis (direct microscopic examination and culture. RESULTS: Otomycosis was diagnosed in 19.4% of the patients. Patient age varied from 2 to 66 years (an average of 23.5 years of age, and 60% of otomycosis cases were seen in women between 2 to 20 years of age. Chronic otitis, previous antibiotic therapy and the lack of cerumen were predisposing factors; itching, otalgia, otorrhea and hypoacusis were the symptoms reported by the patients. The most frequently isolated species were C. albicans (30%, C. parapsilosis (20%, A. niger (20%, A. flavus (10%, A. fumigatus (5%, C. tropicalis (5%, Trichosporon asahii (5% and Scedosporium apiospermum (5%. CONCLUSIONS: Otomycosis is endemic in João Pessoa-PB. Clinical exam and mycological studies are important for diagnostic purposes because otomycosis symptoms are not specific.Otomicose é uma infecção fúngica do conduto auditivo externo com poucos estudos sobre sua real frequência no Brasil. OBJETIVO: Avaliar a frequência e características das otomicoses em pacientes com suspeita clínica de otite externa. DESENHO DO ESTUDO: Estudo retrospectivo com corte transversal (2000-2006. MATERIAL E MÉTODOS: 103 pacientes foram atendidos para diagnóstico micológico (exame microscópico direto e cultivo. RESULTADOS: Otomicoses foram diagnosticadas em 19,4% dos pacientes. A idade desses pacientes variou de 2 a 66 anos (média de 23,5 anos e 60% das otomicoses foram observadas em mulheres entre 2 a 20 anos de idade. Otite crônica, antibioticoterapia prévia e ausência de cerume foram os fatores predisponentes e prurido otológico, otalgia

  7. Coronal Mass Ejections

    CERN Document Server

    Kunow, H; Linker, J. A; Schwenn, R; Steiger, R

    2006-01-01

    It is well known that the Sun gravitationally controls the orbits of planets and minor bodies. Much less known, however, is the domain of plasma fields and charged particles in which the Sun governs a heliosphere out to a distance of about 15 billion kilometers. What forces activates the Sun to maintain this power? Coronal Mass Ejections (CMEs) and their descendants are the troops serving the Sun during high solar activity periods. This volume offers a comprehensive and integrated overview of our present knowledge and understanding of Coronal Mass Ejections (CMEs) and their descendants, Interplanetary CMEs (ICMEs). It results from a series of workshops held between 2000 and 2004. An international team of about sixty experimenters involved e.g. in the SOHO, ULYSSES, VOYAGER, PIONEER, HELIOS, WIND, IMP, and ACE missions, ground observers, and theoreticians worked jointly on interpreting the observations and developing new models for CME initiations, development, and interplanetary propagation. The book provides...

  8. Evolving Coronal Holes and Interplanetary Erupting Stream ...

    Indian Academy of Sciences (India)

    prominences, have a significantly higher rate of occurrence in the vicinity of coronal .... coronal holes due to the birth of new holes or the growth of existing holes. .... Statistics of newly formed coronal hole areas (NFOCHA) associated with ...

  9. Un análisis retrospectivo de cavernomatosis de la vena porta en Chile: II. Hemorragia, tratamiento y pronóstico

    OpenAIRE

    Harris D., Paul; Brinck M., Patricio

    1999-01-01

    Objetivo: El tratamiento de la hipertensión portal de origen prehepático en niños es motivo de controversia. El objetivo de este estudio retrospectivo fue analizar la evolución, tratamiento y morbimortalidad de 34 niños con cavermomatosis de la vena porta. Pacientes y método: Se analizó la evolución antropométrica y hematológica, las características del sangramiento digestivo, el tratamiento médico, endoscópico y quirúrgico, y la morbimortalidad. Resultados: El 74% de los niños presentó uno o...

  10. Coronal heating via nanoflares

    International Nuclear Information System (INIS)

    Poletto, G.; Kopp, R.

    1993-01-01

    It has been recently proposed that the coronae of single late-type main sequence stars represent the radiative output from a large number of tiny energy release events, the so-called nanoflares. Although this suggestion is attractive and order of magnitude estimates of the physical parameters involved in the process are consistent with available data, nanoflares have not yet been observed and theoretical descriptions of these phenomena are still very crude. In this paper we examine the temporal behavior of a magnetic flux tube subject to the repeated occurrence of energy release events, randomly distributed in time, and we show that an originally empty cool loop may, in fact, reach typical coronal density and temperature values via nanoflare heating. By choosing physical parameters appropriate to solar conditions we also explore the possibilities for observationally detecting nanoflares. Although the Sun is the only star where nanoflares might be observed, present instrumentation appears to be inadequate for this purpose

  11. Interpretation of coronal synoptic observations

    International Nuclear Information System (INIS)

    Munro, R.H.; Fisher, R.R.

    1986-01-01

    Three-dimensional reconstruction techniques used to determine coronal density distributions from synoptic data are complicated and time consuming to employ. Current techniques also assume time invariant structures and thus mix both temporal and spatial variations present in the coronal data. The observed distribution of polarized brightness, pB, and brightness, B, of coronal features observed either at eclipses or with coronagraphs depends upon both the three-dimensional distribution of electron density within the structure and the location of the feature with respect to the plane-of-the-sky. By theoretically studying the signature of various coronal structures as they would appear during a limb transit, it is possible to recognize these patterns in real synoptic data as well as estimate temporal evolutionary effects

  12. Solar Coronal Plumes

    Directory of Open Access Journals (Sweden)

    Giannina Poletto

    2015-12-01

    Full Text Available Polar plumes are thin long ray-like structures that project beyond the limb of the Sun polar regions, maintaining their identity over distances of several solar radii. Plumes have been first observed in white-light (WL images of the Sun, but, with the advent of the space era, they have been identified also in X-ray and UV wavelengths (XUV and, possibly, even in in situ data. This review traces the history of plumes, from the time they have been first imaged, to the complex means by which nowadays we attempt to reconstruct their 3-D structure. Spectroscopic techniques allowed us also to infer the physical parameters of plumes and estimate their electron and kinetic temperatures and their densities. However, perhaps the most interesting problem we need to solve is the role they cover in the solar wind origin and acceleration: Does the solar wind emanate from plumes or from the ambient coronal hole wherein they are embedded? Do plumes have a role in solar wind acceleration and mass loading? Answers to these questions are still somewhat ambiguous and theoretical modeling does not provide definite answers either. Recent data, with an unprecedented high spatial and temporal resolution, provide new information on the fine structure of plumes, their temporal evolution and relationship with other transient phenomena that may shed further light on these elusive features.

  13. PONDEROMOTIVE ACCELERATION IN CORONAL LOOPS

    Energy Technology Data Exchange (ETDEWEB)

    Dahlburg, R. B.; Obenschain, K. [LCP and FD, Naval Research Laboratory, Washington, DC 20375 (United States); Laming, J. M. [Space Science Division, Naval Research Laboratory, Washington, DC 20375 (United States); Taylor, B. D. [AFRL Eglin AFB, Pensacola, FL 32542 (United States)

    2016-11-10

    Ponderomotive acceleration has been asserted to be a cause of the first ionization potential (FIP) effect, the well-known enhancement in abundance by a factor of 3–4 over photospheric values of elements in the solar corona with FIP less than about 10 eV. It is shown here by means of numerical simulations that ponderomotive acceleration occurs in solar coronal loops, with the appropriate magnitude and direction, as a “by-product” of coronal heating. The numerical simulations are performed with the HYPERION code, which solves the fully compressible three-dimensional magnetohydrodynamic equations including nonlinear thermal conduction and optically thin radiation. Numerical simulations of coronal loops with an axial magnetic field from 0.005 to 0.02 T and lengths from 25,000 to 75,000 km are presented. In the simulations the footpoints of the axial loop magnetic field are convected by random, large-scale motions. There is a continuous formation and dissipation of field-aligned current sheets, which act to heat the loop. As a consequence of coronal magnetic reconnection, small-scale, high-speed jets form. The familiar vortex quadrupoles form at reconnection sites. Between the magnetic footpoints and the corona the reconnection flow merges with the boundary flow. It is in this region that the ponderomotive acceleration occurs. Mirroring the character of the coronal reconnection, the ponderomotive acceleration is also found to be intermittent.

  14. PONDEROMOTIVE ACCELERATION IN CORONAL LOOPS

    International Nuclear Information System (INIS)

    Dahlburg, R. B.; Obenschain, K.; Laming, J. M.; Taylor, B. D.

    2016-01-01

    Ponderomotive acceleration has been asserted to be a cause of the first ionization potential (FIP) effect, the well-known enhancement in abundance by a factor of 3–4 over photospheric values of elements in the solar corona with FIP less than about 10 eV. It is shown here by means of numerical simulations that ponderomotive acceleration occurs in solar coronal loops, with the appropriate magnitude and direction, as a “by-product” of coronal heating. The numerical simulations are performed with the HYPERION code, which solves the fully compressible three-dimensional magnetohydrodynamic equations including nonlinear thermal conduction and optically thin radiation. Numerical simulations of coronal loops with an axial magnetic field from 0.005 to 0.02 T and lengths from 25,000 to 75,000 km are presented. In the simulations the footpoints of the axial loop magnetic field are convected by random, large-scale motions. There is a continuous formation and dissipation of field-aligned current sheets, which act to heat the loop. As a consequence of coronal magnetic reconnection, small-scale, high-speed jets form. The familiar vortex quadrupoles form at reconnection sites. Between the magnetic footpoints and the corona the reconnection flow merges with the boundary flow. It is in this region that the ponderomotive acceleration occurs. Mirroring the character of the coronal reconnection, the ponderomotive acceleration is also found to be intermittent.

  15. Solar Coronal Structure Study

    Science.gov (United States)

    Nitta, Nariaki; Bruner, Marilyn E.; Saba, Julia; Strong, Keith; Harvey, Karen

    2000-01-01

    The subject of this investigation is to study the physics of the solar corona through the analysis of the EUV and UV data produced by two flights (12 May 1992 and 25 April 1994) of the Lockheed Solar Plasma Diagnostics Experiment (SPDE) sounding rocket payload, in combination with Yohkoh and ground-based data. Each rocket flight produced both spectral and imaging data. These joint datasets are useful for understanding the physical state of various features in the solar atmosphere at different heights ranging from the photosphere to the corona at the time of the, rocket flights, which took place during the declining phase of a solar cycle, 2-4 years before the minimum. The investigation is narrowly focused on comparing the physics of small- and medium-scale strong-field structures with that of large-scale, weak fields. As we close th is investigation, we have to recall that our present position in the understanding of basic solar physics problems (such as coronal heating) is much different from that in 1995 (when we proposed this investigation), due largely to the great success of SOHO and TRACE. In other words, several topics and techniques we proposed can now be better realized with data from these missions. For this reason, at some point of our work, we started concentrating on the 1992 data, which are more unique and have more supporting data. As a result, we discontinued the investigation on small-scale structures, i.e., bright points, since high-resolution TRACE images have addressed more important physics than SPDE EUV images could do. In the final year, we still spent long time calibrating the 1992 data. The work was complicated because of the old-fashioned film, which had problems not encountered with more modern CCD detectors. After our considerable effort on calibration, we were able to focus on several scientific topics, relying heavily on the SPDE UV images. They include the relation between filaments and filament channels, the identification of hot

  16. Coronal Mass Ejections An Introduction

    CERN Document Server

    Howard, Timothy

    2011-01-01

    In times of growing technological sophistication and of our dependence on electronic technology, we are all affected by space weather. In its most extreme form, space weather can disrupt communications, damage and destroy spacecraft and power stations, and increase radiation exposure to astronauts and airline passengers. Major space weather events, called geomagnetic storms, are large disruptions in the Earth’s magnetic field brought about by the arrival of enormous magnetized plasma clouds from the Sun. Coronal mass ejections (CMEs) contain billions of tons of plasma and hurtle through space at speeds of several million miles per hour. Understanding coronal mass ejections and their impact on the Earth is of great interest to both the scientific and technological communities. This book provides an introduction to coronal mass ejections, including a history of their observation and scientific revelations, instruments and theory behind their detection and measurement, and the status quo of theories describing...

  17. Observational Analysis of Coronal Fans

    Science.gov (United States)

    Talpeanu, D.-C.; Rachmeler, L; Mierla, Marilena

    2017-01-01

    Coronal fans (see Figure 1) are bright observational structures that extend to large distances above the solar surface and can easily be seen in EUV (174 angstrom) above the limb. They have a very long lifetime and can live up to several Carrington rotations (CR), remaining relatively stationary for many months. Note that they are not off-limb manifestation of similarly-named active region fans. The solar conditions required to create coronal fans are not well understood. The goal of this research was to find as many associations as possible of coronal fans with other solar features and to gain a better understanding of these structures. Therefore, we analyzed many fans and created an overview of their properties. We present the results of this statistical analysis and also a case study on the longest living fan.

  18. Coronal ``Wave'': Magnetic Footprint of a Coronal Mass Ejection?

    Science.gov (United States)

    Attrill, Gemma D. R.; Harra, Louise K.; van Driel-Gesztelyi, Lidia; Démoulin, Pascal

    2007-02-01

    We investigate the properties of two ``classical'' EUV Imaging Telescope (EIT) coronal waves. The two source regions of the associated coronal mass ejections (CMEs) possess opposite helicities, and the coronal waves display rotations in opposite senses. We observe deep core dimmings near the flare site and also widespread diffuse dimming, accompanying the expansion of the EIT wave. We also report a new property of these EIT waves, namely, that they display dual brightenings: persistent ones at the outermost edge of the core dimming regions and simultaneously diffuse brightenings constituting the leading edge of the coronal wave, surrounding the expanding diffuse dimmings. We show that such behavior is consistent with a diffuse EIT wave being the magnetic footprint of a CME. We propose a new mechanism where driven magnetic reconnections between the skirt of the expanding CME magnetic field and quiet-Sun magnetic loops generate the observed bright diffuse front. The dual brightenings and the widespread diffuse dimming are identified as innate characteristics of this process.

  19. Estenosis traqueal: Estudio preliminar

    Directory of Open Access Journals (Sweden)

    Rafael Pinilla González

    2000-12-01

    Full Text Available Se realizó un estudio retrospectivo y descriptivo con la utilización de los expedientes clínicos de 5 pacientes con estenosis traqueal, mayoritariamente como consecuencia de intubación prolongada, y en el que se tuvo en cuenta aspectos relacionados con el diagnóstico, el tratamiento y las complicaciones. Existió un predominio del sexo femenino y edad media de 44,6 años. La intubación prolongada de origen diverso fue la causa de la estenosis en 4 de los 5 pacientes y en 1 fue posterior a la reparación de lesión traqueal yatrógena. La instalación de la estenosis tuvo lugar entre 8 días y 3 meses. La tomografía lineal en 3 pacientes y en 2 la radiografía simple de tráquea anteroposterior y lateral verificaron el diagnóstico. La endoscopia traqueobronquial preoperatoria fue de utilidad en la caracterización de la estenosis. En todos los pacientes se realizó tratamiento quirúrgico al resecar el área estenótica con posterior anastomosis terminoterminal y fijación del cuello en flexión durante 8 días como promedio. Dos pacientes mostraron granulomas en el nivel de la línea de sutura, los cuales fueron tratados por vacuolización con láser. No se reportó mortalidad en la muestra estudiadaA retrospective and descriptive study was conducted by using the medical histories of 5 patients with tracheal stenosis, mostly as a result of prolongued intubation. Aspects connected with the diagnosis, treatment and complications were taken into account. It was observed a predominance of females and an average age of 44.6. Prolongued intubation of different origin was the cause of stenosis in 4 of the 5 patients, whereas in the other it occurred after the reparation of the tracheal and athrogenous lesion. The installation of stenosis took place between 8 days and 3 months. Lineal tomography in 3 patients and anteroposterior and lateral simple X-ray of the trachea in 2 confirmed the diagnosis. Preoperative tracheobronchial endoscopy was

  20. The dynamics of coronal magnetic structures

    International Nuclear Information System (INIS)

    Weber, W.

    1978-01-01

    An analysis is made of the evolution of coronal magnetic fields due to the interaction with the solar wind. An analysis of the formation of coronal streamers, arising as a result of the stretching of bipolar fields, is given. Numerical simulations of the formation of coronal streamers are presented. Fast-mode shocks as triggers of microturbulence in the solar corona are discussed

  1. Dynamics of Coronal Hole Boundaries

    Energy Technology Data Exchange (ETDEWEB)

    Higginson, A. K.; Zurbuchen, T. H. [Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI 48109 (United States); Antiochos, S. K.; DeVore, C. R. [Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Wyper, P. F. [Universities Space Research Association, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771 (United States)

    2017-03-10

    Remote and in situ observations strongly imply that the slow solar wind consists of plasma from the hot, closed-field corona that is released onto open magnetic field lines. The Separatrix Web theory for the slow wind proposes that photospheric motions at the scale of supergranules are responsible for generating dynamics at coronal-hole boundaries, which result in the closed plasma release. We use three-dimensional magnetohydrodynamic simulations to determine the effect of photospheric flows on the open and closed magnetic flux of a model corona with a dipole magnetic field and an isothermal solar wind. A rotational surface motion is used to approximate photospheric supergranular driving and is applied at the boundary between the coronal hole and helmet streamer. The resulting dynamics consist primarily of prolific and efficient interchange reconnection between open and closed flux. The magnetic flux near the coronal-hole boundary experiences multiple interchange events, with some flux interchanging over 50 times in one day. Additionally, we find that the interchange reconnection occurs all along the coronal-hole boundary and even produces a lasting change in magnetic-field connectivity in regions that were not driven by the applied motions. Our results show that these dynamics should be ubiquitous in the Sun and heliosphere. We discuss the implications of our simulations for understanding the observed properties of the slow solar wind, with particular focus on the global-scale consequences of interchange reconnection.

  2. MHD aspects of coronal transients

    International Nuclear Information System (INIS)

    Anzer, U.

    1979-10-01

    If one defines coronal transients as events which occur in the solar corona on rapid time scales (< approx. several hours) then one would have to include a large variety of solar phenomena: flares, sprays, erupting prominences, X-ray transients, white light transients, etc. Here we shall focus our attention on the latter two phenomena. (orig.) 891 WL/orig. 892 RDG

  3. Prueba de tolerancia oral a la glucosa modificada en puérperas como diagnóstico retrospectivo de diabetes gestacional

    Directory of Open Access Journals (Sweden)

    Joel Cárdenas

    2004-03-01

    Full Text Available Objetivo: Determinar la relación entre la prueba de tolerancia oral a la glucosa (PTOG en puérperas con macrosomia fetal y plantearla como método de diagnóstico retrospectivo para diabetes gestacional. Diseño de estudio: Estudio clínico, de corte transversal, analítico, casos y controles. Material y Métodos: Estudio de 142 puérperas, 71 con recién nacidos macrosómicos y 71 con recién nacidos con pesos en percentiles de la normalidad. Se realizó una PTOG modificada de dos horas (basal, 1h y 2 h, con 100 g de glucosa, entre las primeras 8 y 48 horas posparto (positivo si [glicemia 2h - basal] + [glicemia 1h - basal] 110 mg/dL. Se utilizó el SPSS 10,0 para crear la base de datos y realizar el análisis estadístico: análisis univariado, bivariado para evaluar la hipótesis, y finalmente un análisis multivariado. Resultados: La PTOG anormal resultó un factor de riesgo para macrosomia fetal, con un odds ratio ajustado de 5,9; IC95% 2,6-13,4. Se encontró asociación entre antecedente de macrosomia fetal, odds ratio 15,7; IC95% 1,9-123,6 y control prenatal odds ratio 5,7; IC95% 1,2-26,8. Conclusión: Existe relación entre la PTOG en puérperas y macrosomia fetal, que puede ser usada como prueba diagnóstica retrospectiva de diabetes gestacional.

  4. The Coronal Place; Why is It Special?

    Directory of Open Access Journals (Sweden)

    Azhar Alkazwini

    2017-10-01

    Full Text Available To prove the existence of arguments about the exact place that can bear the term ‘coronal’, it would be enough to check the explanatory dictionary’s entry. There are different arguments regarding the exact place of coronal. In this paper, some of the linguistic evidence regarding the coronal place shall be mentioned. Then, I shall discuss the classes of coronal that lend support to the fact that coronal place is believed to be special, and that is by discussing the different typologies of coronal consonants and giving their description.

  5. An equatorial coronal hole at solar minimum

    Science.gov (United States)

    Bromage, B. J. I.; DelZanna, G.; DeForest, C.; Thompson, B.; Clegg, J. R.

    1997-01-01

    The large transequatorial coronal hole that was observed in the solar corona at the end of August 1996 is presented. It consists of a north polar coronal hole called the 'elephant's trunk or tusk'. The observations of this coronal hole were carried out with the coronal diagnostic spectrometer onboard the Solar and Heliospheric Observatory (SOHO). The magnetic field associated with the equatorial coronal hole is strongly connected to that of the active region at its base, resulting in the two features rotating at almost the same rate.

  6. Coronal Seismology: The Search for Propagating Waves in Coronal Loops

    Science.gov (United States)

    Schad, Thomas A.; Seeley, D.; Keil, S. L.; Tomczyk, S.

    2007-05-01

    We report on Doppler observations of the solar corona obtained in the Fe XeXIII 1074.7nm coronal emission line with the HAO Coronal Multi-Channel Polarimeter (CoMP) mounted on the NSO Coronal One Shot coronagraph located in the Hilltop Facility of NSO/Sacramento Peak. The COMP is a tunable filtergraph instrument that records the entire corona from the edge of the occulting disk at approximately 1.03 Rsun out to 1.4 Rsun with a spatial resolution of about 4” x 4”. COMP can be rapidly scanned through the spectral line while recording orthogonal states of linear and circular polarization. The two dimensional spatial resolution allows us to correlate temporal fluctuations observed in one part of the corona with those seen at other locations, in particular along coronal loops. Using cross spectral analysis we find that the observations reveal upward propagating waves that are characterized by Doppler shifts with rms velocities of 0.3 km/s, peak wave power in the 3-5 mHz frequency range, and phase speeds 1-3 Mm/s. The wave trajectories are consistent with the direction of the magnetic field inferred from the linear polarization measurements. We discuss the phase and coherence of these waves as a function of height in the corona and relate our findings to previous observations. The observed waves appear to be Alfvenic in character. "Thomas Schad was supported through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program." Daniel Seeley was supported through the National Solar Observatory Research Experience for Teachers (RET) site program, which is funded by the National Science Foundation RET program.

  7. Procedimiento para el análisis retrospectivo y prospectivo de sistemas lecheros

    Directory of Open Access Journals (Sweden)

    J.A Herrera

    Full Text Available Con el objetivo de proponer un procedimiento integrador para el análisis retrospectivo y prospectivo de sistemas lecheros, se realizó una investigación documental basada en una revisión bibliográfica narrativa. La información provino de dos tipos de fuente: primaria y secundaria, mientras que la estrategia de búsqueda se basó en combinaciones de palabras clave. El procedimiento, que consistió en realizar 22 operaciones de manera ordenada, se basó en el enfoque de ingeniería de sistema y contempló las cuatro dimensiones generales (productiva, económica, social y ambiental que definen la sostenibilidad de los sistemas agropecuarios. Se utilizó este enfoque por considerar que el análisis de dichos sistemas se debe orientar al examen holístico de lo que en ellos ocurre, así como a proponer soluciones concretas con bases científicas. Los resultados demostraron que la secuencia de operaciones propuesta puede ser considerada como un procedimiento útil para realizar el análisis retrospectivo y prospectivo de sistemas lecheros, con un enfoque sistémico e integrador que permite interrelacionar la caracterización del sistema de producción de leche en pastoreo, el análisis de la eficiencia y el diseño de alternativas tecnológicas para la mejora de este.

  8. Polarization of Coronal Forbidden Lines

    Energy Technology Data Exchange (ETDEWEB)

    Li, Hao; Qu, Zhongquan [Yunnan Observatories, Chinese Academy of Sciences, Kunming, Yunnan 650011 (China); Landi Degl’Innocenti, Egidio, E-mail: sayahoro@ynao.ac.cn [Dipartimento di Astronomia e Scienza dello Spazio, Università di Firenze, Largo E. Fermi 2, I-50125 Firenze (Italy)

    2017-03-20

    Since the magnetic field is responsible for most manifestations of solar activity, one of the most challenging problems in solar physics is the diagnostics of solar magnetic fields, particularly in the outer atmosphere. To this end, it is important to develop rigorous diagnostic tools to interpret polarimetric observations in suitable spectral lines. This paper is devoted to analyzing the diagnostic content of linear polarization imaging observations in coronal forbidden lines. Although this technique is restricted to off-limb observations, it represents a significant tool to diagnose the magnetic field structure in the solar corona, where the magnetic field is intrinsically weak and still poorly known. We adopt the quantum theory of polarized line formation developed in the framework of the density matrix formalism, and synthesize images of the emergent linear polarization signal in coronal forbidden lines using potential-field source-surface magnetic field models. The influence of electronic collisions, active regions, and Thomson scattering on the linear polarization of coronal forbidden lines is also examined. It is found that active regions and Thomson scattering are capable of conspicuously influencing the orientation of the linear polarization. These effects have to be carefully taken into account to increase the accuracy of the field diagnostics. We also found that linear polarization observation in suitable lines can give valuable information on the long-term evolution of the magnetic field in the solar corona.

  9. Estudio EPIFARM

    Directory of Open Access Journals (Sweden)

    Martín Morales A

    2010-12-01

    Full Text Available INTRODUCCIÓN Los farmacéuticos comunitarios pueden ser un importante primer punto de contacto con los pacientes con disfunción eréctil (DE, pero hasta la fecha no hay ningún estudio sobre las características de los hombres que acuden a un farmacéutico solicitando consejo o tratamiento para la DE. OBJETIVO Caracterizar los perfiles de los hombres que solicitan tratamiento para la DE en la farmacia, con o sin receta de inhibidores de la fosfodiesterasa tipo 5 (iPDE5. MÉTODOS Entre septiembre y noviembre de 2008 se realizó un estudio observacional, transversal y multicéntrico en farmacias comunitarias de España. De aquellos hombres que solicitaban consejo o tratamiento para la DE, cada investigador reclutó un paciente que tenía receta médica de iPDE5 y otro que acudía sin receta médica. Los farmacéuticos del estudio completaron un cuestionario de datos demográficos, clínicos y conductuales del paciente, incluido el Cuestionario de salud sexual para varones (Sexual Health Inventory for Men. VARIABLES PRINCIPALES Características demográficas y respuestas a los cuestionarios. RESULTADOS 574 farmacéuticos seleccionaron a 1.147 pacientes, de los cuales 1.113 fueron incluidos en el análisis. No se observaron diferencias estadísticas entre los grupos en cuanto al peso, la hipertensión, la diabetes mellitus, la hipercolesterolemia, la dislipidemia, la depresión o el estrés. Tampoco se observaron diferencias estadísticas respecto a la gravedad de la DE (p = 0,7892 ni a la proporción de hombres sin DE en cada grupo (p = 0,5755. En ambos grupos, los pacientes habían presentado síntomas de DE durante una media de veintiséis meses antes de la primera consulta a un profesional sanitario. Para el 60,2% de los pacientes incluidos en el grupo sin receta, la visita a la farmacia fue la primera ocasión en la que habían hablado de su DE con un profesional sanitario, y el 50% de aquellos que habían hablado previamente de la DE lo hab

  10. RIESGOS OBSTETRICOS EN EL EMBARAZO ADOLESCENTE: ESTUDIO COMPARATIVO DE RESULTADOS OBSTETRICOS Y PERINATALES CON PACIENTES EMBARAZADAS ADULTAS

    OpenAIRE

    Díaz,Angélica; Sanhueza R,Pablo; Yaksic B,Nicole

    2002-01-01

    Se presenta un estudio retrospectivo y comparativo, a través de una muestra obtenida en forma aleatoria, de la evolución materna y resultados obstétricos de las pacientes adolescentes embarazadas atendidas en el Servicio de Obstetricia y Ginecología del Hospital Salvador, en comparación con un grupo control obtenido en el mismo Servicio y período de estudio. Se analizan diversas variables, y se hace una completa revisión del tema en base a la literatura nacional y extranjera.

  11. Síndrome icterícia em gatos: revisão de literatura e estudo retrospectivo

    OpenAIRE

    OLIVEIRA, Roberta Alencar de; DANIEL, Alexandre Gonçalves Teixeira; RECHE JUNIOR, Archivaldo

    2008-01-01

    Icterícia é uma alteração clínica comumente encontrada nos felinos, causada por níveis excessivos de bilirrubina na circulação e nos tecidos, indicando hemólise grave ou doença hepatobiliar. Este trabalho é composto por uma revisão da literatura e um estudo retrospectivo sobre a síndrome icterícia em felinos e suas principais causas: lipidose hepática, colângio-hepatite, tríade felina e micoplasmose felina. O estudo retrospectivo foi realizado utilizando-se das informações contidas nos prontu...

  12. Space weather and coronal mass ejections

    CERN Document Server

    Howard, Tim

    2013-01-01

    Space weather has attracted a lot of attention in recent times. Severe space weather can disrupt spacecraft, and on Earth can be the cause of power outages and power station failure. It also presents a radiation hazard for airline passengers and astronauts. These ""magnetic storms"" are most commonly caused by coronal mass ejections, or CMES, which are large eruptions of plasma and magnetic field from the Sun that can reach speeds of several thousand km/s. In this SpringerBrief, Space Weather and Coronal Mass Ejections, author Timothy Howard briefly introduces the coronal mass ejection, its sc

  13. “ERA ÓBVIO QUE ISSO IRIA ACONTECER”: CONSIDERAÇÕES SOBRE O VIÉS RETROSPECTIVO

    Directory of Open Access Journals (Sweden)

    Bruno Stefani Ferreira de Oliveira

    2017-10-01

    Full Text Available O viés retrospectivo é o fenômeno de perceber e avaliar eventos diferentemente, uma vez que eles tenham ocorrido. Dada uma falha cognitiva, pessoas tendem a ter distorções da memória e a produzir falsas sensações de inevitabilidade e previsibilidade. Os objetivos deste trabalho foram fazer uma revisão de literatura do viés retrospectivo e discutir as implicações teóricas e práticas do tema. Uma pesquisa, realizada nas principais bases de dados do país, não encontrou nenhum artigo relacionado com o tema. A partir de uma seleção das principais pesquisas internacionais sobre o assunto, foi feita uma análise que mostrou os níveis cognitivos do viés retrospectivo, suas implicações e as estratégias usadas para atenuar o viés. Nas considerações finais, são discutidos o impacto e a importância do conhecimento desse fenômeno no dia a dia de tomadores de decisão e cidadãos, assim como a necessidade de se explorar o tema em pesquisas nacionais.

  14. Coronal Magnetism and Forward Solarsoft Idl Package

    Science.gov (United States)

    Gibson, S. E.

    2014-12-01

    The FORWARD suite of Solar Soft IDL codes is a community resource for model-data comparison, with a particular emphasis on analyzing coronal magnetic fields. FORWARD may be used both to synthesize a broad range of coronal observables, and to access and compare to existing data. FORWARD works with numerical model datacubes, interfaces with the web-served Predictive Science Inc MAS simulation datacubes and the Solar Soft IDL Potential Field Source Surface (PFSS) package, and also includes several analytic models (more can be added). It connects to the Virtual Solar Observatory and other web-served observations to download data in a format directly comparable to model predictions. It utilizes the CHIANTI database in modeling UV/EUV lines, and links to the CLE polarimetry synthesis code for forbidden coronal lines. FORWARD enables "forward-fitting" of specific observations, and helps to build intuition into how the physical properties of coronal magnetic structures translate to observable properties.

  15. Tratamento cirúrgico da laringomalácia grave: estudo retrospectivo de 11 casos

    Directory of Open Access Journals (Sweden)

    José Antonio Pinto

    2013-10-01

    Full Text Available A laringomalácia é a anomalia congênita da laringe mais frequente, sendo responsável por cerca de 60% a 75% dos casos de estridor congênito. Apesar de seu curso benigno e autolimitado, 10% dos casos necessitam de intervenção. Atualmente, as supraglotoplastias são consideradas o tratamento padrão da laringomalácia grave. OBJETIVO: Descrever a experiência adquirida pelos autores no tratamento cirúrgico dos pacientes com laringomalácia grave. Metodologia: Estudo retrospectivo. MÉTODO: Os prontuários de 11 casos consecutivos de laringomalácia grave, submetidos ao tratamento cirúrgico entre 2003 e 2012, foram analisados quanto à idade, gênero, sintomas, doenças associadas, técnica cirúrgica adotada, tempo de extubação, complicações cirúrgicas, tempo de internação e evolução clínica. RESULTADOS: Dos 11 casos de laringomalácia grave, seis pacientes (54,5% foram operados com o uso do laser de CO2 e em cinco pacientes (45,5% foram realizadas a técnica a frio. Apenas um paciente (9,1% necessitou reabordagem cirúrgica. Não foram observados casos de complicações cirúrgicas. Todos os pacientes apresentaram melhora clínica importante. CONCLUSÃO: A supraglotoplastia mostrou-se um procedimento eficaz e seguro no tratamento da laringomalácia grave.

  16. Estudo retrospectivo-sistemático da matriz extracelular de tumores mamários caninos

    Directory of Open Access Journals (Sweden)

    Ana Maria Cristina Rabello Pinto da Fonseca Martins

    2002-01-01

    Full Text Available A finalidade do presente trabalho foi efetuar um estudo retrospectivo, de 1932 à 1999 , afim de se estabelecer a casuística desses tumores nos arquivos do Departamento de Patologia da Faculdade de Medicina Veterinária - USP , bem como a freqüência de desmoplasia, metaplasia cartilaginosa e óssea em 578 desses tumores. Entre os 537 tumores malignos, 13.05% foram adenocarcinomas tubulares simples, 3.91% foram adenocarcinomas tubulares compostos, 7.26% adenocarcinomas papilíferos simples, 4.28% adenocarcinomas papilíferos compostos, 23.27% cistoadenocarcinomas papilíferos simples, 8.37% cistoadenocarcinomas papilíferos compostos, 16.38% adenocarcinomas sólidos simples, 6.70% adenocarcinomas sólidos compostos, 2.04% carcinomas de células espinhosas simples, 1.11% carcinomas de células espinhosas compostos, 2.79% carcinomas mucinosos ,8.19% carcinomas anaplásicos ,0.93% carcinomas escamosos, 1.30% fibrossarcomas,.0.18% condrossarcoma, 0.18% osteossarcoma e entre os 41 tumores benignos ,51.21% foram adenomas, 12.19% cistadenomas pailíferos,7.31% papilomas, 4.87% fibroadenomas e 24.39% foram fibroadenomas. Tanto a desmoplasia como a metaplasia foi um achado freqüente nas neoplasias benignas e malignas, mas foram mais freqüentes entre os adenocarcinomas tubulares compostos: 38% apresentaram desmoplasia, 57% metaplasia cartilaginosa e 28% metaplasia óssea. Entre as neoplasias benignas, adenoma apresentou a maior frequência: 14 % com desmoplasia, 29% com metaplasia cartilaginosa e 24% com metaplasia óssea. Os resultados deste estudo enfatizam a complexidade da inter-relação entre as macromoléculas da matriz extracelular e as células tumorais.

  17. COMPOSITION OF CORONAL MASS EJECTIONS

    Energy Technology Data Exchange (ETDEWEB)

    Zurbuchen, T. H.; Weberg, M.; Lepri, S. T. [Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI (United States); Von Steiger, R. [International Space Science Institute, Bern (Switzerland); Mewaldt, R. A. [California Institute of Technology, Pasadena, CA (United States); Antiochos, S. K. [Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD (United States)

    2016-07-20

    We analyze the physical origin of plasmas that are ejected from the solar corona. To address this issue, we perform a comprehensive analysis of the elemental composition of interplanetary coronal mass ejections (ICMEs) using recently released elemental composition data for Fe, Mg, Si, S, C, N, Ne, and He as compared to O and H. We find that ICMEs exhibit a systematic abundance increase of elements with first ionization potential (FIP) < 10 eV, as well as a significant increase of Ne as compared to quasi-stationary solar wind. ICME plasmas have a stronger FIP effect than slow wind, which indicates either that an FIP process is active during the ICME ejection or that a different type of solar plasma is injected into ICMEs. The observed FIP fractionation is largest during times when the Fe ionic charge states are elevated above Q {sub Fe} > 12.0. For ICMEs with elevated charge states, the FIP effect is enhanced by 70% over that of the slow wind. We argue that the compositionally hot parts of ICMEs are active region loops that do not normally have access to the heliosphere through the processes that give rise to solar wind. We also discuss the implications of this result for solar energetic particles accelerated during solar eruptions and for the origin of the slow wind itself.

  18. Coronal rain in magnetic bipolar weak fields

    Science.gov (United States)

    Xia, C.; Keppens, R.; Fang, X.

    2017-07-01

    Aims: We intend to investigate the underlying physics for the coronal rain phenomenon in a representative bipolar magnetic field, including the formation and the dynamics of coronal rain blobs. Methods: With the MPI-AMRVAC code, we performed three dimensional radiative magnetohydrodynamic (MHD) simulation with strong heating localized on footpoints of magnetic loops after a relaxation to quiet solar atmosphere. Results: Progressive cooling and in-situ condensation starts at the loop top due to radiative thermal instability. The first large-scale condensation on the loop top suffers Rayleigh-Taylor instability and becomes fragmented into smaller blobs. The blobs fall vertically dragging magnetic loops until they reach low-β regions and start to fall along the loops from loop top to loop footpoints. A statistic study of the coronal rain blobs finds that small blobs with masses of less than 1010 g dominate the population. When blobs fall to lower regions along the magnetic loops, they are stretched and develop a non-uniform velocity pattern with an anti-parallel shearing pattern seen to develop along the central axis of the blobs. Synthetic images of simulated coronal rain with Solar Dynamics Observatory Atmospheric Imaging Assembly well resemble real observations presenting dark falling clumps in hot channels and bright rain blobs in a cool channel. We also find density inhomogeneities during a coronal rain "shower", which reflects the observed multi-stranded nature of coronal rain. Movies associated to Figs. 3 and 7 are available at http://www.aanda.org

  19. MULTIDIMENSIONAL MODELING OF CORONAL RAIN DYNAMICS

    Energy Technology Data Exchange (ETDEWEB)

    Fang, X.; Xia, C.; Keppens, R. [Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, B-3001 Leuven (Belgium)

    2013-07-10

    We present the first multidimensional, magnetohydrodynamic simulations that capture the initial formation and long-term sustainment of the enigmatic coronal rain phenomenon. We demonstrate how thermal instability can induce a spectacular display of in situ forming blob-like condensations which then start their intimate ballet on top of initially linear force-free arcades. Our magnetic arcades host a chromospheric, transition region, and coronal plasma. Following coronal rain dynamics for over 80 minutes of physical time, we collect enough statistics to quantify blob widths, lengths, velocity distributions, and other characteristics which directly match modern observational knowledge. Our virtual coronal rain displays the deformation of blobs into V-shaped features, interactions of blobs due to mostly pressure-mediated levitations, and gives the first views of blobs that evaporate in situ or are siphoned over the apex of the background arcade. Our simulations pave the way for systematic surveys of coronal rain showers in true multidimensional settings to connect parameterized heating prescriptions with rain statistics, ultimately allowing us to quantify the coronal heating input.

  20. MULTIDIMENSIONAL MODELING OF CORONAL RAIN DYNAMICS

    International Nuclear Information System (INIS)

    Fang, X.; Xia, C.; Keppens, R.

    2013-01-01

    We present the first multidimensional, magnetohydrodynamic simulations that capture the initial formation and long-term sustainment of the enigmatic coronal rain phenomenon. We demonstrate how thermal instability can induce a spectacular display of in situ forming blob-like condensations which then start their intimate ballet on top of initially linear force-free arcades. Our magnetic arcades host a chromospheric, transition region, and coronal plasma. Following coronal rain dynamics for over 80 minutes of physical time, we collect enough statistics to quantify blob widths, lengths, velocity distributions, and other characteristics which directly match modern observational knowledge. Our virtual coronal rain displays the deformation of blobs into V-shaped features, interactions of blobs due to mostly pressure-mediated levitations, and gives the first views of blobs that evaporate in situ or are siphoned over the apex of the background arcade. Our simulations pave the way for systematic surveys of coronal rain showers in true multidimensional settings to connect parameterized heating prescriptions with rain statistics, ultimately allowing us to quantify the coronal heating input.

  1. Disfunção intestinal em pacientes com lesão cerebral decorrente de acidente vascular cerebral e traumatismo craniencefálico: estudo retrospectivo de uma série de casos

    Directory of Open Access Journals (Sweden)

    Cinthia Carlos Dourado

    2012-01-01

    Full Text Available La disfunción del intestino es una queja común entre los pacientes con daño cerebral debido a una lesión cerebral traumática y accidente cerebrovascular. Este estudio tuvo como objetivo investigar la prevalencia de disfunción del intestino (incontinencia y constipación en pacientes con daño cerebral debido a una lesión cerebral traumática y accidente cerebrovascular admitidos para la rehabilitación. Este es un estudio retrospectivo de una serie de casos a partir del análisis de los datos de 138 expedientes de los pacientes ingresados en el primer semestre de 2009. La prevalencia de disfunción del intestino fue de 41%, siendo 33 (24% incontinencia anal y 37 (27%, constipación. El comprometimiento motor, ayuda a la movilidad, cambios en la memoria y la comunicación se asocian con la presencia de la incontinencia anal. La prevalencia de disfunción del intestino es alta en esta población, identificar en forma temprana los factores relacionados, y promover el reentrenamiento intestinal pueden ayudar a mejorar la calidad de sus vidas.

  2. Histerectomía puerperal: Estudio de 14 años

    OpenAIRE

    Fuentes Gonzalez, Leonardo; Enriguez Domínguez, Bárbara

    2005-01-01

    Se realizó un estudio retrospectivo, longitudinal y descriptivo en el hospital docente "Julio Trigo López", con el objetivo de caracterizar las histerectomías puerperales en el período comprendido entre Mayo de 1989 a diciembre del 2002 . El universo estuvo comprendido por 99 pacientes para una tasa de incidencia de 21,8 por 100 000 nacimientos. Se encontró que la cesárea se destaca como proceder de riesgo en el 55,7 % de los casos. Las causas fundamentales que llevaron a estas pacientes a la...

  3. Estudio comparativo de las maloclusiones de clase III tratadas con y sin cirugía

    OpenAIRE

    Martínez Asúnsolo, Pascual

    2014-01-01

    El objetivo de la presente tesis fue determinar si existen diferencias en la inclinación de los incisivos superiores e inferiores en pacientes de clase III tratados con cirugía o únicamente con “camuflaje ortodóncico”, así como su repercusión en la relación esquelética final. Para ello se realizó un estudio clínico comparativo y retrospectivo en la unidad docente de Ortodoncia del departamento de Estomatología de la Universidad de Valencia. La muestra consistió en 56 pacientes que cump...

  4. Estudo retrospectivo de 66 casos de urolitíase obstrutiva em ovinos

    Directory of Open Access Journals (Sweden)

    Janaina Azevedo Guimarães

    2012-09-01

    Full Text Available Objetivou-se realizar um estudo retrospectivo dos principais achados epidemiológicos, clínicos, patológicos e laboratoriais de ovinos acometidos por urolitíase obstrutiva, atendidos na Clínica de Bovinos, Campus Garanhuns/ UFRPE. Para isso, foram analisadas 66 fichas clínicas de ovinos, todos machos não castrados, com idade entre dois meses e cinco anos. A maioria dos casos (79,63% ocorreu na época chuvosa. A maioria dos animais (87,88% era criada intensivamente e todos eram alimentados com concentrados. Os sinais clínicos mais importantes foram as manifestações de dor, congestão de mucosas, hipertermia e aumento da tensão abdominal associados a obstrução do trato urinário. Metade dos animais apresentou obstrução total da uretra. Destes, 69,70% morreram, enquanto nos casos de obstrução parcial, 30,30% morreram. Nos exames laboratoriais verificou-se neutrofilia e desvio à esquerda regenerativo, hiperfibrinogenemia e azotemia. Na urinálise constatou-se hematúria em 89,29% dos casos e pH ácido em 46,43%. Na sedimentoscopia predominaram hemácias, leucócitos, células de descamação do epitélio uretral e cristais de urato amorfo. Os achados necroscópicos renais mais frequentes foram pielonefrite (61,54% dos casos e hidronefrose (50%. Nos ureteres foram visualizados ureterite e hidroureter. Na bexiga foi mais evidente a cistite hemorrágica difusa (50% e a presença de urólitos (57,69%. Na uretra observaram-se urólitos (61,54% e uretrite hemorrágica difusa (57,69%. Quanto à composição dos urólitos predominaram os compostos por oxalato de cálcio hidratado. Conclui-se que no Agreste de Pernambuco a urolitiase é uma doença importante de ovinos, com alta letalidade, estando associada à alimentação rica em concentrados e sal mineral.

  5. Introduction of hind foot coronal alignment view

    International Nuclear Information System (INIS)

    Moon, Il Bong; Jeon, Ju Seob; Yoon, Kang Cheol; Choi, Nam Kil; Kim, Seung Kook

    2006-01-01

    Accurate clinical evaluation of the alignment of the calcaneus relative to the tibia in the coronal plane is essential in the evaluation and treatment of hind foot pathologic condition. Previously described standard anteroposterior, lateral, and oblique radiographic methods of the foot or ankle do not demonstrate alignment of the tibia relation to the calcaneus in the coronal plane. The purpose of this study was to introduce hind foot coronal alignment view. Both feet were imaged simultaneously on an elevated, radiolucent foot stand equipment. Both feet stood on a radiolucent platform with equal weight on both feet. Both feet are located foot axis longitudinal perpendicular to the platform. Silhouette tracing around both feet are made, and line is then drawn to bisect the silhouette of the second toe and the outline of the heel. The x-ray beam is angled down approximately 15 .deg. to 20 .deg. This image described tibial axis and medial, lateral tuberosity of calcaneus. Calcaneus do not rotated. The view is showed by talotibial joint space. Although computed tomographic and magnetic resonance imaging techniques are capable of demonstrating coronal hind foot alignment, they lack usefulness in most clinical situations because the foot is imaged in a non-weight bearing position. But hind foot coronal alignment view is obtained for evaluating position changing of inversion, eversion of the hind foot and varus, valgus deformity of calcaneus

  6. Free Magnetic Energy and Coronal Heating

    Science.gov (United States)

    Winebarger, Amy; Moore, Ron; Falconer, David

    2012-01-01

    Previous work has shown that the coronal X-ray luminosity of an active region increases roughly in direct proportion to the total photospheric flux of the active region's magnetic field (Fisher et al. 1998). It is also observed, however, that the coronal luminosity of active regions of nearly the same flux content can differ by an order of magnitude. In this presentation, we analyze 10 active regions with roughly the same total magnetic flux. We first determine several coronal properties, such as X-ray luminosity (calculated using Hinode XRT), peak temperature (calculated using Hinode EIS), and total Fe XVIII emission (calculated using SDO AIA). We present the dependence of these properties on a proxy of the free magnetic energy of the active region

  7. The first coronation churches of medieval Serbia

    Directory of Open Access Journals (Sweden)

    Kalić Jovanka

    2017-01-01

    Full Text Available The medieval ceremony of coronation as a rule took place in the most important church of a realm. The sites of the coronation of Serbian rulers before the establishment of the Žiča monastery church as the coronation church of Serbian kings in the first half of the thirteenth century have not been reliably identified so far. Based on the surviving medieval sources and the archaeological record, this paper provides background information about the titles of Serbian rulers prior to the creation of the Nemanjić state, and proposes that Stefan, son of the founder of the Nemanjić dynasty, was crowned king (1217 in the church of St Peter in Ras.

  8. A contemporary view of coronal heating.

    Science.gov (United States)

    Parnell, Clare E; De Moortel, Ineke

    2012-07-13

    Determining the heating mechanism (or mechanisms) that causes the outer atmosphere of the Sun, and many other stars, to reach temperatures orders of magnitude higher than their surface temperatures has long been a key problem. For decades, the problem has been known as the coronal heating problem, but it is now clear that 'coronal heating' cannot be treated or explained in isolation and that the heating of the whole solar atmosphere must be studied as a highly coupled system. The magnetic field of the star is known to play a key role, but, despite significant advancements in solar telescopes, computing power and much greater understanding of theoretical mechanisms, the question of which mechanism or mechanisms are the dominant supplier of energy to the chromosphere and corona is still open. Following substantial recent progress, we consider the most likely contenders and discuss the key factors that have made, and still make, determining the actual (coronal) heating mechanism (or mechanisms) so difficult.

  9. DIRECT OBSERVATION OF SOLAR CORONAL MAGNETIC FIELDS BY VECTOR TOMOGRAPHY OF THE CORONAL EMISSION LINE POLARIZATIONS

    International Nuclear Information System (INIS)

    Kramar, M.; Lin, H.; Tomczyk, S.

    2016-01-01

    We present the first direct “observation” of the global-scale, 3D coronal magnetic fields of Carrington Rotation (CR) Cycle 2112 using vector tomographic inversion techniques. The vector tomographic inversion uses measurements of the Fe xiii 10747 Å Hanle effect polarization signals by the Coronal Multichannel Polarimeter (CoMP) and 3D coronal density and temperature derived from scalar tomographic inversion of Solar Terrestrial Relations Observatory (STEREO)/Extreme Ultraviolet Imager (EUVI) coronal emission lines (CELs) intensity images as inputs to derive a coronal magnetic field model that best reproduces the observed polarization signals. While independent verifications of the vector tomography results cannot be performed, we compared the tomography inverted coronal magnetic fields with those constructed by magnetohydrodynamic (MHD) simulations based on observed photospheric magnetic fields of CR 2112 and 2113. We found that the MHD model for CR 2112 is qualitatively consistent with the tomography inverted result for most of the reconstruction domain except for several regions. Particularly, for one of the most noticeable regions, we found that the MHD simulation for CR 2113 predicted a model that more closely resembles the vector tomography inverted magnetic fields. In another case, our tomographic reconstruction predicted an open magnetic field at a region where a coronal hole can be seen directly from a STEREO-B/EUVI image. We discuss the utilities and limitations of the tomographic inversion technique, and present ideas for future developments

  10. De hiperfrecuentadora a abuela esclava: Estudio de un caso de sobrecarga del cuidador desde el Síndrome de la Abuela Esclava de Guijarro Morales

    OpenAIRE

    García González, J.; Rosillo Castro, D.; Salazar, I.R.; Raygal Fernández, P.J.; Lázaro Meca, R.S.; Cánovas Gaspar, J.P.

    2011-01-01

    El trabajo tiene como objetivo conocer el perfil de una paciente hiperfrecuentadora que acude al servicio de urgencias hospitalario 299 ocasiones en 3 años y analizarlo a través del marco teórico del síndrome de la abuela esclava de Guijarro Morales. Concluimos, analizando su perfil de demanda (estudio epidemiológico retrospectivo) y a través de una entrevista semiestructurada (estudio descriptivo cualitativo), que la paciente sufre el síndrome de la abuela esclava. Por último realizamos una ...

  11. Estudio comparativo del tratamiento ortésico en las fracturas toraco-lumbosacras según la gravedad del trauma

    OpenAIRE

    Manzone,Patricio; Stefanizzi,Julio; Ávalos,Eduardo Mariño; Barranco,Silvia Manzone; Ihlenfeld,Claudia

    2011-01-01

    OBJETIVO: Determinar si la gravedad del trauma en lesiones toracolumbosacras mayores estables permite decidir la selección del tipo de ortesis en un tratamiento ortopédico. MÉTODOS: Estudio Retrospectivo de casos 12/1990 - 12/2006 (16 años). Criterios de Selección: 1) Seguimiento mínimo: 2 años. 2) Estudios radiológicos convencionales completos. 3) Ausencia de Litigio. 4) Tratamiento ortésico con TLSO a medida para los traumas de alta energía cinética y con ortesis prefabricadas para los de b...

  12. EMBARAZO Y MATERNIDAD ADOLESCENTE EN BOGOTÁ Y MUNICIPIOS ALEDAÑOS: CONSECUENCIAS EN EL ESTUDIO, ESTADO CIVIL, ESTRUCTURA FAMILIAR, OCUPACION Y PROYECTO DE VIDA

    OpenAIRE

    Salazar, Andrés; Rodríguez, Luisa Fernanda; Daza, Rodrigo Antonio

    2007-01-01

    El embarazo adolescente constituye un evento vital de importantes repercusiones en distintas dimensiones de la mujer: estudio, estructura familiar, ocupación, proyecto de vida y estado civil. De ahí que se busque indagar sobre sus consecuencias sociales y económicas y verificar si tiene comportamiento hereditario. Con este fin se realizó, como criterio de inclusión para la muestra, un estudio de tipo retrospectivo transversal para el cual se entrevistó a 20 madres adolescentes, según las defi...

  13. Estudio de la morbimortalidad en pacientes intervenidos de estenosis carotídea que precisan transfusión sanguínea

    OpenAIRE

    Ibáñez Maraña, María Antonia

    2016-01-01

    Se trata de un estudio retrospectivo en pacientes intervenidos de estenosis carotídea mediante la realización de endarterectomía carotídea. Estos pacientes han sido operados en el Hospital Clínico Universitario de Valladolid, en el periodo comprendido entre enero del 2012 y enero del 2014, ambos incluidos. Todos los pacientes operados de estenosis carotídea en dicho periodo fueron incluidos en el estudio, ya que no se precisa seguimiento de los mismos. Se analiza la morbimortalidad...

  14. Radio emission from coronal and interplanetary shocks

    International Nuclear Information System (INIS)

    Cane, H.V.

    1987-01-01

    Observational data on coronal and interplanetary (IP) type II burst events associated with shock-wave propagation are reviewed, with a focus on the past and potential future contributions of space-based observatories. The evidence presented by Cane (1983 and 1984) in support of the hypothesis that the coronal (metric) and IP (kilometric) bursts are due to different shocks is summarized, and the fast-drift kilometric events seen at the same time as metric type II bursts (and designated shock-accelerated or shock-associated events) are characterized. The need for further observations at 0.5-20 MHz is indicated. 20 references

  15. C4. Pneumonia adquirida na comunidade (PAC: estudo retrospectivo num hospital central

    Directory of Open Access Journals (Sweden)

    A. Oliveira

    2003-11-01

    Full Text Available A PAC é uma importante causa de morbilidade e mortalidade nos doentes hospitalizados. O objectivo deste estudo foi analisar a etiologia, factores de risco, tratamento e mortalidade da PAC no internamento. Procedemos a um estudo retrospectivo de 246 doentes, admitidos no nosso Departamento com o diagnóstico de PAC num período de 24 meses. A média etária foi de 58,9 anos e 61% eram do sexo masculino. Em 48,6% existiam comorbilidades. Na radiografia torácica havia envolvimento multilobar em 17,1%, padrão alveolar em 66,7% e derrame pleural em 18,3%.Os agentes etiológicos foram pesquisados em 195 doentes (75,9% e foram positivos em 57 (29,2%: 11% das hemoculturas (19/173; 30% dos exames culturais de expectoração (48/160 e 10.4% das serologias e antigenúria para Legionella (7/67 foram positivos. Nos doentes com etiologia bacteriana o agente etiológico mais frequente foi S. pneumoniae (47%, seguindo-se os Gram-negativos (26% e H. Influenza (18%.A amoxicilina/clavulanato (82,9% e macrólidos (68,1% foram os antibióticos mais usados. Houve associação de antibióticos em 61,6% dos doentes. A duração média do tratamento foi de 12 dias. Em 93% dos doentes assistiu-se a evolução favorável. A mortalidade foi de 5,1%.Concluimos que o S. pneumoniae continua a ser o agente etiológico mais frequente de PAC. A escolha terapêutica esteve de acordo com as guidelines internacionais e o regime terapêutico mostrou-se adequado tendo a maioria das PAC evolução favorável com baixa mortalidade. : CAP is an important cause of morbidity and mortality in hospitalized patients. The aim of this study was to analyze etiology, risk factors, treatment and mortality of CAP. We conducted a retrospective analysis of clinical data from 246 patients admitted to our Department with CAP diagnosis throughout an 24 month period.The patients were in average age 58,9 years old and 61% were male. In 48,6% significant co-morbidities were found. On chest X-ray there

  16. Solar Wind Associated with Near Equatorial Coronal Hole M ...

    Indian Academy of Sciences (India)

    2015-05-25

    May 25, 2015 ... coronal hole and solar wind. For both the wavelength bands, we also com- pute coronal hole radiative energy near the earth and it is found to be of similar order as that of solar wind energy. However, for the wavelength. 193 Å, owing to almost similar magnitudes of energy emitted by coronal hole and ...

  17. Higher-speed coronal mass ejections and their geoeffectiveness

    Science.gov (United States)

    Singh, A. K.; Bhargawa, Asheesh; Tonk, Apeksha

    2018-06-01

    We have attempted to examine the ability of coronal mass ejections to cause geoeffectiveness. To that end, we have investigated total 571 cases of higher-speed (> 1000 km/s) coronal mass ejection events observed during the years 1996-2012. On the basis of angular width (W) of observance, events of coronal mass ejection were further classified as front-side or halo coronal mass ejections (W = 360°); back-side halo coronal mass ejections (W = 360°); partial halo (120°mass ejections were much faster and more geoeffective in comparison of partial halo and non-halo coronal mass ejections. We also inferred that the front-sided halo coronal mass ejections were 67.1% geoeffective while geoeffectiveness of partial halo coronal mass ejections and non-halo coronal mass ejections were found to be 44.2% and 56.6% respectively. During the same period of observation, 43% of back-sided CMEs showed geoeffectiveness. We have also investigated some events of coronal mass ejections having speed > 2500 km/s as a case study. We have concluded that mere speed of coronal mass ejection and their association with solar flares or solar activity were not mere criterion for producing geoeffectiveness but angular width of coronal mass ejections and their originating position also played a key role.

  18. Magnetic Topology of Coronal Hole Linkages

    Science.gov (United States)

    Titov, V. S.; Mikic, Z.; Linker, J. A.; Lionello, R.; Antiochos, S. K.

    2010-01-01

    In recent work, Antiochos and coworkers argued that the boundary between the open and closed field regions on the Sun can be extremely complex with narrow corridors of open ux connecting seemingly disconnected coronal holes from the main polar holes, and that these corridors may be the sources of the slow solar wind. We examine, in detail, the topology of such magnetic configurations using an analytical source surface model that allows for analysis of the eld with arbitrary resolution. Our analysis reveals three important new results: First, a coronal hole boundary can join stably to the separatrix boundary of a parasitic polarity region. Second, a single parasitic polarity region can produce multiple null points in the corona and, more important, separator lines connecting these points. Such topologies are extremely favorable for magnetic reconnection, because it can now occur over the entire length of the separators rather than being con ned to a small region around the nulls. Finally, the coronal holes are not connected by an open- eld corridor of finite width, but instead are linked by a singular line that coincides with the separatrix footprint of the parasitic polarity. We investigate how the topological features described above evolve in response to motion of the parasitic polarity region. The implications of our results for the sources of the slow solar wind and for coronal and heliospheric observations are discussed.

  19. Simulating coronal condensation dynamics in 3D

    Science.gov (United States)

    Moschou, S. P.; Keppens, R.; Xia, C.; Fang, X.

    2015-12-01

    We present numerical simulations in 3D settings where coronal rain phenomena take place in a magnetic configuration of a quadrupolar arcade system. Our simulation is a magnetohydrodynamic simulation including anisotropic thermal conduction, optically thin radiative losses, and parametrised heating as main thermodynamical features to construct a realistic arcade configuration from chromospheric to coronal heights. The plasma evaporation from chromospheric and transition region heights eventually causes localised runaway condensation events and we witness the formation of plasma blobs due to thermal instability, that evolve dynamically in the heated arcade part and move gradually downwards due to interchange type dynamics. Unlike earlier 2.5D simulations, in this case there is no large scale prominence formation observed, but a continuous coronal rain develops which shows clear indications of Rayleigh-Taylor or interchange instability, that causes the denser plasma located above the transition region to fall down, as the system moves towards a more stable state. Linear stability analysis is used in the non-linear regime for gaining insight and giving a prediction of the system's evolution. After the plasma blobs descend through interchange, they follow the magnetic field topology more closely in the lower coronal regions, where they are guided by the magnetic dips.

  20. The physical structure of coronal holes

    International Nuclear Information System (INIS)

    Pneuman, G.W.

    1978-11-01

    The longitudinal geometrical structure of solar wind streams as observed at the orbit of earth is governed by two mechanisms - solar rotation and, most importantly, the geometry of the inner coronal magnetic fields. Here, we study the influence of the latter for the polar coronal hole observed by Skylab in 1973 and modeled by Munro and Jackson (1977). The influence of coronal heating on the properties of the solar wind in this geometry is also investigated. To do this, a crude exponentially damped heating function similar to that used by Kopp and Orrall (1976) is introduced into the solar wind equations. We find that increased heating produces higher temperatures in the inner corona but has little effect upon the temperature at 1 A.U. However, the density at 1 A.U. is increased significantly due to the increase in scale height. The most surprising consequence of coronal heating is its effect on the solar wind velocity, being that the velocity at 1 A.U. is actually decreased by heating in the inner corona. Physical reasons for this effect are discussed. (orig./WL) [de

  1. Solar wind acceleration in coronal holes

    International Nuclear Information System (INIS)

    Kopp, R.A.

    1978-01-01

    Past attempts to explain the large solar wind velocities in high speed streams by theoretical models of the expansion have invoked either extended nonthermal heating of the corona, heat flux inhibition, or direct addition of momentum to the expanding coronal plasma. Several workers have shown that inhibiting the heat flux at low coronal densities is probably not adequate to explain quantitatively the observed plasma velocities in high speed streams. It stressed that, in order to account for both these large plasma velocities and the low densities found in coronal holes (from which most high speed streams are believed to emanate), extended heating by itself will not suffice. One needs a nonthermal mechanism to provide the bulk acceleration of the high wind plasma close to the sun, and the most likely candidate at present is direct addition of the momentum carried by outward-propagating waves to the expanding corona. Some form of momentum addition appears to be absolutely necessary if one hopes to build quantitatively self-consistent models of coronal holes and high speed solar wind streams

  2. Evolving Coronal Holes and Interplanetary Erupting Stream ...

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Coronal holes and interplanetary disturbances are important aspects of the physics of the Sun and heliosphere. Interplanetary disturbances are identified as an increase in the density turbulence compared with the ambient solar wind. Erupting stream disturbances are transient large-scale structures of ...

  3. Role of Magnetic Carpet in Coronal Heating

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... One of the fundamental questions in solar physics is how the solar corona maintains its high temperature of several million Kelvin above photosphere with a temperature of 6000 K. Observations show that solar coronal heating problem is highly complex with many different facts. It is likely that different ...

  4. Mechanisms of Coronal Heating S. R. Verma

    Indian Academy of Sciences (India)

    Abstract. The Sun is a mysterious star. The high temperature of the chromosphere and corona present one of the most puzzling problems of solar physics. Observations show that the solar coronal heating problem is highly complex with many different facts. It is likely that different heating mechanisms are at work in solar ...

  5. Radiotherapy treatment results of bladder cancer: study of 458 patients. Resultados del tratamiento radioterapico en cancer de vejiga: estudio retrospectivo de 458 pacientes

    Energy Technology Data Exchange (ETDEWEB)

    Vara Santos, J.; Torre Tomas, A. de la; Romero Fernandez, J.; Regueiro Otero, C.; Clavo Varas, B.; Magallan Sebastian, R.; Valcarcel Sancho, F.; Polo Tolosana, E.; Aragon de la Cruz, G.

    1994-01-01

    Between 1964 to 1990, 458 patients diagnosed of bladder cancer have been treated with radical radiotherapy in our department. The 5-years and 10-years actuarial survival rates were 37% and 27% respectively. The 5-years and 10-years actuarial local control rates, evaluated in 404 patients, were 41% and 38%. In regard to survival, T stage (p=0.013), advanced intravesical extension or multicentrity (p>0.0001), and squamous differentiation (p<0.0001), reached statistical significance as adverse prognostic factors. In 248 patients, with invasive transitional carcinoma, radical radiotherapy alone was used. In this group of patients, T stage (p=0.006) and advanced intravesical extension or multicentrity (p=0.0002) were adverse prognostic factors for survival. Our results suggest that radical radiotherapy must be considered and alternative to surgery in management of bladder cancer. On the basis of prognostic factors evidenced in this series a subgroup of patients with low probability of survival when treated with exclusive radiotherapy are defined. This patients must be included in clinical research protocols. (Author) 44 refs.

  6. Nonlinear Force-free Coronal Magnetic Stereoscopy

    Energy Technology Data Exchange (ETDEWEB)

    Chifu, Iulia; Wiegelmann, Thomas; Inhester, Bernd, E-mail: chifu@mps.mpg.de [Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, D-37077 Göttingen (Germany)

    2017-03-01

    Insights into the 3D structure of the solar coronal magnetic field have been obtained in the past by two completely different approaches. The first approach are nonlinear force-free field (NLFFF) extrapolations, which use photospheric vector magnetograms as boundary condition. The second approach uses stereoscopy of coronal magnetic loops observed in EUV coronal images from different vantage points. Both approaches have their strengths and weaknesses. Extrapolation methods are sensitive to noise and inconsistencies in the boundary data, and the accuracy of stereoscopy is affected by the ability of identifying the same structure in different images and by the separation angle between the view directions. As a consequence, for the same observational data, the 3D coronal magnetic fields computed with the two methods do not necessarily coincide. In an earlier work (Paper I) we extended our NLFFF optimization code by including stereoscopic constrains. The method was successfully tested with synthetic data, and within this work, we apply the newly developed code to a combined data set from SDO /HMI, SDO /AIA, and the two STEREO spacecraft. The extended method (called S-NLFFF) contains an additional term that monitors and minimizes the angle between the local magnetic field direction and the orientation of the 3D coronal loops reconstructed by stereoscopy. We find that when we prescribe the shape of the 3D stereoscopically reconstructed loops, the S-NLFFF method leads to a much better agreement between the modeled field and the stereoscopically reconstructed loops. We also find an appreciable decrease by a factor of two in the angle between the current and the magnetic field. This indicates the improved quality of the force-free solution obtained by S-NLFFF.

  7. INTERCHANGE RECONNECTION AND CORONAL HOLE DYNAMICS

    International Nuclear Information System (INIS)

    Edmondson, J. K.; Antiochos, S. K.; DeVore, C. R.; Lynch, B. J.; Zurbuchen, T. H.

    2010-01-01

    We investigate the effect of magnetic reconnection between open and closed fields, often referred to as 'interchange' reconnection, on the dynamics and topology of coronal hole boundaries. The most important and most prevalent three-dimensional topology of the interchange process is that of a small-scale bipolar magnetic field interacting with a large-scale background field. We determine the evolution of such a magnetic topology by numerical solution of the fully three-dimensional MHD equations in spherical coordinates. First, we calculate the evolution of a small-scale bipole that initially is completely inside an open field region and then is driven across a coronal hole boundary by photospheric motions. Next the reverse situation is calculated in which the bipole is initially inside the closed region and driven toward the coronal hole boundary. In both cases, we find that the stress imparted by the photospheric motions results in deformation of the separatrix surface between the closed field of the bipole and the background field, leading to rapid current sheet formation and to efficient reconnection. When the bipole is inside the open field region, the reconnection is of the interchange type in that it exchanges open and closed fields. We examine, in detail, the topology of the field as the bipole moves across the coronal hole boundary and find that the field remains well connected throughout this process. Our results, therefore, provide essential support for the quasi-steady models of the open field, because in these models the open and closed flux are assumed to remain topologically distinct as the photosphere evolves. Our results also support the uniqueness hypothesis for open field regions as postulated by Antiochos et al. On the other hand, the results argue against models in which open flux is assumed to diffusively penetrate deeply inside the closed field region under a helmet streamer. We discuss the implications of this work for coronal observations.

  8. DARK JETS IN SOLAR CORONAL HOLES

    Energy Technology Data Exchange (ETDEWEB)

    Young, Peter R. [College of Science, George Mason University, 4400 University Drive, Fairfax, VA 22030 (United States)

    2015-03-10

    A new solar feature termed a dark jet is identified from observations of an extended solar coronal hole that was continuously monitored for over 44 hr by the Extreme Ultraviolet Imaging Spectrometer on board the Hinode spacecraft in 2011 February 8–10 as part of Hinode Operation Plan No. 177 (HOP 177). Line of sight (LOS) velocity maps derived from the coronal Fe xii λ195.12 emission line, formed at 1.5 MK, revealed a number of large-scale, jet-like structures that showed significant blueshifts. The structures had either weak or no intensity signal in 193 Å filter images from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory, suggesting that the jets are essentially invisible to imaging instruments. The dark jets are rooted in bright points and occur both within the coronal hole and at the quiet Sun–coronal hole boundary. They exhibit a wide range of shapes, from narrow columns to fan-shaped structures, and sometimes multiple jets are seen close together. A detailed study of one dark jet showed LOS speeds increasing along the jet axis from 52 to 107 km s{sup −1} and a temperature of 1.2–1.3 MK. The low intensity of the jet was due either to a small filling factor of 2% or to a curtain-like morphology. From the HOP 177 sample, dark jets are as common as regular coronal hole jets, but their low intensity suggests a mass flux around two orders of magnitude lower.

  9. Los estudios longitudinales en la prevención de las enfermedades cardiovasculares

    Directory of Open Access Journals (Sweden)

    Ignacio Balaguer Vintró

    2004-01-01

    Full Text Available Los estudios longitudinales de cohortes bien definidas han contribuido a la identificación de los factores de riesgo de la cardiopatía coronaria y otras complicaciones clínicas de la aterosclerosis. Después de comentar las conclusiones de los estudios de la aterosclerosis experimental y los factores de riesgo sugeridos por el estudio de una serie de infartos de miocardio en adultos jóvenes en comparación con controles apareados, se expone la metodología, el desarrollo y los resultados de los estudios longitudinales realizados en Estados Unidos desde 1949: Twin Cities, Framingham, Pooling Project, Western Collaborative, Puerto Rico, Evans County, NI-HONSAN, San Francisco, Harvard, Bogalusa y CARDIA. Se presta especial atención a las hipótesis propuestas al inicio del estudio de Framingham y a los obstáculos y cambios para continuar el proyecto después de los primeros veinticuatro años. A continuación se expone el Seven Countries Study, ideado y dirigido por Ancel Keys y primer estudio realizado con metodología centralizada en varios países, y los estudios longitudinales realizados en diversos países de Europa: Whitehall, Manresa, París, British Regional, Northwick Park, Caerphilly, Speedwell, PROCAM. Se analiza el papel de los estudios longitudinales en la metodología de los estudios posteriores: hijos e hijas de los participantes en Framingham, estudios longitudinales basados en cuestionarios, estudios de otros posibles factores de riesgo, prevalencia de factores de riesgo en estudios retrospectivos, ensayos de intervención primaria (MRFT, WHO European Collaborative Trial y el de Goteburgo y la participación de los equipos entrenados en el Proyecto MONICA. Se señalan los temas todavía en debate en relación con la metodología y los resultados de los estudios longitudinales: exámenes periódicos de los participantes en las cohortes de los estudios epidemiológicos, cambios en la definición de nuevos casos de accidentes

  10. El homicidio y los homicidas. Estudio descriptivo del homicidio en la provincia de Bizkaia (1992-2013). Características clínicas, médico legales y jurídicas de los homicidas .

    OpenAIRE

    Abasolo Tellería, Ana Eugenia

    2017-01-01

    266 p. Esta tesis busca el estudio descriptivo y retrospectivo, en base a lasexploraciones medico-forenses, de personas acusadas de un delito de homicidioconsumado, en la Audiencia Provincial de Bizkaia, durante el periodo 1992-2013.Se trata de un trabajo que enlaza dos areas del conocimiento: la medicina y elderecho. Al tratarse de un entorno forense, el resultado de las exploraciones tieneconsecuencias legales, en la determinación y graduación de la capacidad de culpabilidado imputabilid...

  11. Demografía industrial: un estudio sobre relocalización de firmas en Colombia, 1995-2012

    Directory of Open Access Journals (Sweden)

    Charle Londoño

    2015-01-01

    Full Text Available Este trabajo realiza un estudio retrospectivo sobre la relocalización de firmas en Colombia. Para ello, se evalúa la incidencia de variables financieras, tributarias, territoriales y de accesibilidad en la relocalización de empresas, utilizando un modelo de regresión logística y una muestra de 36.235 compañías en el periodo 1995-2012. Se encuentra que la tributación es un factor neurálgico para las decisiones de localización.

  12. Coronal Heating: Testing Models of Coronal Heating by Forward-Modeling the AIA Emission of the Ansample of Coronal Loops

    Science.gov (United States)

    Malanushenko, A. V.

    2015-12-01

    We present a systemic exploration of the properties of coronal heating, by forward-modeling the emission of the ensemble of 1D quasi-steady loops. This approximations were used in many theoretical models of the coronal heating. The latter is described in many such models in the form of power laws, relating heat flux through the photosphere or volumetric heating to the strength of the magnetic field and length of a given field line. We perform a large search in the parameter space of these power laws, amongst other variables, and compare the resulting emission of the active region to that observed by AIA. We use a recently developed magnetic field model which uses shapes of coronal loops to guide the magnetic model; the result closely resembles observed structures by design. We take advantage of this, by comparing, in individual sub-regions of the active region, the emission of the active region and its synthetic model. This study allows us to rule out many theoretical models and formulate predictions for the heating models to come.

  13. ANÁLISIS RETROSPECTIVO DEL CARDINOMA CUTÁNEO TIPO BASOCELULAR Y ESCAMOCELULAR EN BOGOTÁ - C0LOMBIA: EPIDEMIOLOGÍA, PREVENCIÓN Y TRATAMIENTO

    Directory of Open Access Journals (Sweden)

    Óscar Iván Barón Estrada

    2009-01-01

    Full Text Available Antecedentes. El carcinoma cutáneo no melanoma del tipo basocelular (CBC y escamocelular (CEC, tiene tasas de incidencia cercanas al 13 por ciento y es el más prevalente en la población blanca. Trae elevada morbilidad para el paciente y altos costos para el sistema de salud, y aunque es la neoplasia maligna mas frecuentemente diagnosticada, en Colombia sólo se tienen estadísticas en instituciones oncológicas, haciendo énfasis principalmente en melanomas. Entre los principales factores de riesgo se encuentra la exposición a los RUVB, tipo de piel, la radiación, el virus del papiloma humano (HPV y su tratamiento incluye medicación tópica, crioterapia, electrofulguración y cirugía. Objetivo. Analizar algunas características epidemiológicas del cáncer cutáneo (CBC - CEC en nuestro medio, estableciendo similitudes y diferencias respecto a la literatura actual. Material y métodos. En la clínica San Pedro Claver se revisaron 202 historias clínicas de pacientes con diagnóstico confirmado de CBC O CEC de 2004 a 2006 en un estudio retrospectivo de serie de casos y se analizaron las variables más comunes como el tipo de lesión, su ubicación, tamaño, patrón histológico y tratamiento. Resultados. Ingresaron en el estudio 112 pacientes, de los cuales cerca del 60 por ciento eran hombres, con una edad media de 69.5 años. El 90 por ciento de las lesiones se localizaban en cara (mejillas, párpados, nariz. Del 70 por ciento de las lesiones que correspondían a CBC el tipo histológico más frecuente fue sólido nodular y del 22 por ciento de lesiones que correspondían a CEC, el moderadamente diferenciado de célula grande fue el más común. Las lesiones tuvieron un tamaño promedio de 2 cm y los procedimientos quirúrgicos más usados fueron resección más injerto (44.1%, seguido de resección más colgajo local (23.5%. El 5 por ciento de los pacientes tenían lesiones previas y uno de cada cuatro tuvo algún tipo de reca

  14. Interplanetary Coronal Mass Ejections detected by HAWC

    Science.gov (United States)

    Lara, Alejandro

    The High Altitude Water Cherenkov (HAWC) observatory is being constructed at the volcano Sierra Negra (4100 m a.s.l.) in Mexico. HAWC’s primary purpose is the study of both: galactic and extra-galactic sources of high energy gamma rays. HAWC will consist of 300 large water Cherenkov detectors (WCD), instrumented with 1200 photo-multipliers. The Data taking has already started while construction continues, with the completion projected for late 2014. The HAWC counting rate will be sensitive to cosmic rays with energies above the geomagnetic cutoff of the site (˜ 8 GV). In particular, HAWC will detect solar energetic particles known as Ground Level Enhancements (GLEs), and the effects of Coronal Mass Ejections on the galactic cosmic ray flux, known as Forbush Decreases. In this paper, we present a description of the instrument and its response to interplanetary coronal mass ejections, and other solar wind large scale structures, observed during the August-December 2013 period.

  15. Solar Coronal Jets: Observations, Theory, and Modeling

    Science.gov (United States)

    Raouafi, N. E.; Patsourakos, S.; Pariat, E.; Young, P. R.; Sterling, A.; Savcheva, A.; Shimojo, M.; Moreno-Insertis, F.; Devore, C. R.; Archontis, V.; hide

    2016-01-01

    Chromospheric and coronal jets represent important manifestations of ubiquitous solar transients, which may be the source of signicant mass and energy input to the upper solar atmosphere and the solar wind. While the energy involved in a jet-like event is smaller than that of nominal solar ares and Coronal Mass Ejections (CMEs), jets share many common properties with these major phenomena, in particular, the explosive magnetically driven dynamics. Studies of jets could, therefore, provide critical insight for understanding the larger, more complex drivers of the solar activity. On the other side of the size-spectrum, the study of jets could also supply important clues on the physics of transients closeor at the limit of the current spatial resolution such as spicules. Furthermore, jet phenomena may hint to basic process for heating the corona and accelerating the solar wind; consequently their study gives us the opportunity to attack a broadrange of solar-heliospheric problems.

  16. Sinonasal polyposis: investigation by direct coronal CT

    International Nuclear Information System (INIS)

    Drutman, J.; Harnsberger, H.R.; Babbel, R.W.; Sonkens, J.W.; Braby, D.

    1994-01-01

    To demonstrate the typical clinical and CT features of sinonasal polyposis, we reviewed the clinical records and preoperative direct coronal CT scans of 35 patients with surgically proven disease. Symptoms included progressive nasal stuffiness (100 %), rhinorrhea (69 %), facial pain (60 %), headache (43 %) and anosmia (17 %). We found associations with rhinitis (46 %), asthma (29 %) and aspirin sensitivity (9 %). Coronal CT features included polypoid masses in the nasal cavity (91 %), partial or complete pansinus opacification (90 %), enlargement of infundibula (89 %), bony attenuation of the ethmoid trabeculae (63 %) and nasal septum (37 %), opacified ethmoid sinuses with convex lateral walls (51 %) and air-fluid levels (43 %). The latter feature correlated with symptoms and signs of acute sinusitis in only 40 % of patients. Recognition of sinonasal polyposis is important to the endoscopic surgeon since it can be the most troubling sinonasal inflammatory disease to manage due to its aggressive nature and tendency to recur despite appropriate treatment. (orig.)

  17. Fracture mechanism of coronal teenage dentin

    Science.gov (United States)

    Panfilov, P. E.; Kabanova, A. V.; Borodin, I. N.; Guo, J.; Zang, Z.

    2017-10-01

    The structure of coronal teenage dentin and the development of cracks in it are studied on microand nanolevels. The material is found to fail according to a ductile mechanism on a microlelvel and according to a ductile-brittle mechanism on a nanoscale. This behavior is similar to the failure of a polyethylene film and rubber, when significant elastic and irreversible deformation precedes crack growth. The viscoelastic behavior can be considered as the reaction of dentin to an applied mechanical load.

  18. Plasma Diagnostics of Coronal Dimming Events

    Science.gov (United States)

    Vanninathan, Kamalam; Veronig, Astrid M.; Dissauer, Karin; Temmer, Manuela

    2018-04-01

    Coronal mass ejections are often associated with coronal dimmings, i.e., transient dark regions that are most distinctly observed in Extreme Ultra-violet wavelengths. Using Atmospheric Imaging Assembly (AIA) data, we apply Differential Emission Measure diagnostics to study the plasma characteristics of six coronal dimming events. In the core dimming region, we find a steep and impulsive decrease of density with values up to 50%–70%. Five of the events also reveal an associated drop in temperature of 5%–25%. The secondary dimming regions also show a distinct decrease in density, but less strong, decreasing by 10%–45%. In both the core and the secondary dimming the density changes are much larger than the temperature changes, confirming that the dimming regions are mainly caused by plasma evacuation. In the core dimming, the plasma density reduces rapidly within the first 20–30 minutes after the flare start and does not recover for at least 10 hr later, whereas the secondary dimming tends to be more gradual and starts to replenish after 1–2 hr. The pre-event temperatures are higher in the core dimming (1.7–2.6 MK) than in the secondary dimming regions (1.6–2.0 MK). Both core and secondary dimmings are best observed in the AIA 211 and 193 Å filters. These findings suggest that the core dimming corresponds to the footpoints of the erupting flux rope rooted in the AR, while the secondary dimming represents plasma from overlying coronal structures that expand during the CME eruption.

  19. The transition region and coronal explorer (TRACE)

    Science.gov (United States)

    Title, Alan; Bruner, M.; Jurcevich, B.; Lemen, J.; Strong, K.; Tarbell, Ted; Wolfson, C. Jacob; Golub, L.; Bookbinder, J.; Fisher, R.

    1995-01-01

    The transition region and coronal explorer (TRACE) NASA small explorer mission and instrument are presented. The TRACE scientific investigation explores the relationships between fine-scale magnetic fields and the associated solar plasma structures. The instrument collects images of solar plasmas at temperatures from 10(exp 4) to 10(exp 7) K with one arcsec spatial resolution. The design specifications of the trace instrument are presented.

  20. A SURVEY OF CORONAL CAVITY DENSITY PROFILES

    International Nuclear Information System (INIS)

    Fuller, J.; Gibson, S. E.

    2009-01-01

    Coronal cavities are common features of the solar corona that appear as darkened regions at the base of coronal helmet streamers in coronagraph images. Their darkened appearance indicates that they are regions of lowered density embedded within the comparatively higher density helmet streamer. Despite interfering projection effects of the surrounding helmet streamer (which we refer to as the cavity rim), Fuller et al. have shown that under certain conditions it is possible to use a Van de Hulst inversion of white-light polarized brightness (pB) data to calculate the electron density of both the cavity and cavity rim plasma. In this article, we apply minor modifications to the methods of Fuller et al. in order to improve the accuracy and versatility of the inversion process, and use the new methods to calculate density profiles for both the cavity and cavity rim in 24 cavity systems. We also examine trends in cavity morphology and how departures from the model geometry affect our density calculations. The density calculations reveal that in all 24 cases the cavity plasma has a flatter density profile than the plasma of the cavity rim, meaning that the cavity has a larger density depletion at low altitudes than it does at high altitudes. We find that the mean cavity density is over four times greater than that of a coronal hole at an altitude of 1.2 R sun and that every cavity in the sample is over twice as dense as a coronal hole at this altitude. Furthermore, we find that different cavity systems near solar maximum span a greater range in density at 1.2 R sun than do cavity systems near solar minimum, with a slight trend toward higher densities for systems nearer to solar maximum. Finally, we found no significant correlation of cavity density properties with cavity height-indeed, cavities show remarkably similar density depletions-except for the two smallest cavities that show significantly greater depletion.

  1. Critical Magnetic Field Strengths for Unipolar Solar Coronal Plumes In Quiet Regions and Coronal Holes?

    Science.gov (United States)

    Avallone, Ellis; Tiwari, Sanjiv K.; Panesar, Navdeep K.; Moore, Ronald L.; Winebarger, Amy

    2017-01-01

    Coronal plumes are bright magnetic funnels that are found in quiet regions and coronal holes that extend high into the solar corona whose lifetimes can last from hours to days. The heating processes that make plumes bright involve the magnetic field at the base of the plume, but their intricacies remain mysterious. Raouafi et al. (2014) infer from observation that plume heating is a consequence of magnetic reconnection at the base, whereas Wang et al. (2016) infer that plume heating is a result of convergence of the magnetic flux at the plume's base, or base flux. Both papers suggest that the base flux in their plumes is of mixed polarity, but do not quantitatively measure the base flux or consider whether a critical magnetic field strength is required for plume production. To investigate the magnetic origins of plume heating, we track plume luminosity in the 171 Å wavelength as well as the abundance and strength of the base flux over the lifetimes of six unipolar coronal plumes. Of these, three are in coronal holes and three are in quiet regions. For this sample, we find that plume heating is triggered when convergence of the base flux surpasses a field strength of approximately 300 - 500 Gauss, and that the luminosity of both quiet region and coronal hole plumes respond similarly to the strength of the magnetic field in the base.

  2. Coronal Heating Observed with Hi-C

    Science.gov (United States)

    Winebarger, Amy R.

    2013-01-01

    The recent launch of the High-Resolution Coronal Imager (Hi-C) as a sounding rocket has offered a new, different view of the Sun. With approx 0.3" resolution and 5 second cadence, Hi-C reveals dynamic, small-scale structure within a complicated active region, including coronal braiding, reconnection regions, Alfven waves, and flows along active region fans. By combining the Hi-C data with other available data, we have compiled a rich data set that can be used to address many outstanding questions in solar physics. Though the Hi-C rocket flight was short (only 5 minutes), the added insight of the small-scale structure gained from the Hi-C data allows us to look at this active region and other active regions with new understanding. In this talk, I will review the first results from the Hi-C sounding rocket and discuss the impact of these results on the coronal heating problem.

  3. Forward Modeling of a Coronal Cavity

    Science.gov (United States)

    Kucera, T. A.; Gibson, S. E.; Schmit, D. J.

    2011-01-01

    We apply a forward model of emission from a coronal cavity in an effort to determine the temperature and density distribution in the cavity. Coronal cavities are long, low-density structures located over filament neutral lines and are often seen as dark elliptical features at the solar limb in white light, EUV and X-rays. When these structures erupt they form the cavity portions of CMEs The model consists of a coronal streamer model with a tunnel-like cavity with elliptical cross-section and a Gaussian variation of height along the tunnel length. Temperature and density can be varied as a function of altitude both in the cavity and streamer. We apply this model to a cavity observed in Aug. 2007 by a wide array of instruments including Hinode/EIS, STEREO/EUVI and SOHO/EIT. Studies such as these will ultimately help us understand the the original structures which erupt to become CMEs and ICMES, one of the prime Solar Orbiter objectives.

  4. Temperature Structure of a Coronal Cavity

    Science.gov (United States)

    Kucera, T. A.; Gibson, S. E.; Schmit, D. J.

    2011-01-01

    we analyze the temperature structure of a coronal cavity observed in Aug. 2007. coronal cavities are long, low-density structures located over filament neutral lines and are often seen as dark elliptical features at the solar limb in white light, EUV and x-rays. when these structures erupt they form the cavity portions of CMEs. It is important to establish the temperature structure of cavities in order to understand the thermodynamics of cavities in relation to their three-dimensional magnetic structure. To analyze the temperature we compare temperature ratios of a series of iron lines observed by the Hinode/EUv Imaging spectrometer (EIS). We also use those lines to constrain a forward model of the emission from the cavity and streamer. The model assumes a coronal streamer with a tunnel-like cavity with elliptical cross-section and a Gaussian variation of height along the tunnel lenth. Temperature and density can be varied as a function of altitude both in the cavity and streamer. The general cavity morphology and the cavity and streamer density have already been modeled using data from STEREO's SECCHI/EUVI and Hinode/EIS (Gibson et al 2010 and Schmit & Gibson 2011).

  5. Solar origins of coronal mass ejections

    Science.gov (United States)

    Kahler, Stephen

    1987-01-01

    The large scale properties of coronal mass ejections (CMEs), such as morphology, leading edge speed, and angular width and position, have been cataloged for many events observed with coronagraphs on the Skylab, P-78, and SMM spacecraft. While considerable study has been devoted to the characteristics of the SMEs, their solar origins are still only poorly understood. Recent observational work has involved statistical associations of CMEs with flares and filament eruptions, and some evidence exists that the flare and eruptive-filament associated CMEs define two classes of events, with the former being generally more energetic. Nevertheless, it is found that eruptive-filament CMEs can at times be very energetic, giving rise to interplanetary shocks and energetic particle events. The size of the impulsive phase in a flare-associated CME seems to play no significant role in the size or speed of the CME, but the angular sizes of CMEs may correlate with the scale sizes of the 1-8 angstrom x-ray flares. At the present time, He 10830 angstrom observations should be useful in studying the late development of double-ribbon flares and transient coronal holes to yield insights into the CME aftermath. The recently available white-light synoptic maps may also prove fruitful in defining the coronal conditions giving rise to CMEs.

  6. [Development of electroforming apparatus for coronal restoration].

    Science.gov (United States)

    Watanabe, M; Sawada, T; Ukiya, M

    1989-03-01

    As dental technologies become highly developed, techniques have been more diversified. From as aspect of prosthodontic practice, both esthetic and functional requirements are emphasized for coronal restoration and consequently, these should be considered in the routine procedure. In fabrication of coronal restorations, metal, porcelain and resin are commonly used, and there exists the various disadvantages for metal cast method due to complicated processes by using different dental materials. Therefore, an electroforming apparatus was developed by us to replace the conventional procedure by a cathode rotary system. It was applied for coronal restorations to allow an electroforming directly on a working model. An experiment was successfully conducted to apply for a veneer crown on abutment tooth of upper central incisor on plaster model. The results were obtained as follows, 1. It was become possible to construct a metal framework by the electroforming. 2. Metal framework can be constructed on the same working model without a duplication of it. 3. The combined system for cathode rotation and liquid circulation could shorten the electroposition time, and allows a high current density extending to 50 A/dm2.

  7. SUNQUAKE GENERATION BY CORONAL MAGNETIC RESTRUCTURING

    Energy Technology Data Exchange (ETDEWEB)

    Russell, A. J. B.; Mooney, M. K. [School of Science and Engineering, University of Dundee, Dundee DD1 4HN (United Kingdom); Leake, J. E. [Naval Research Laboratory, Washington, DC 20375 (United States); Hudson, H. S. [Space Sciences Lab, University of California Berkeley, Berkeley, CA 94720 (United States)

    2016-11-01

    Sunquakes are the surface signatures of acoustic waves in the Sun’s interior that are produced by some but not all flares and coronal mass ejections (CMEs). This paper explores a mechanism for sunquake generation by the changes in magnetic field that occur during flares and CMEs, using MHD simulations with a semiempirical FAL-C atmosphere to demonstrate the generation of acoustic waves in the interior in response to changing magnetic tilt in the corona. We find that Alfvén–sound resonance combined with the ponderomotive force produces acoustic waves in the interior with sufficient energy to match sunquake observations when the magnetic field angle changes of the order of 10° in a region where the coronal field strength is a few hundred gauss or more. The most energetic sunquakes are produced when the coronal field is strong, while the variation of magnetic field strength with height and the timescale of the change in tilt are of secondary importance.

  8. SUNQUAKE GENERATION BY CORONAL MAGNETIC RESTRUCTURING

    International Nuclear Information System (INIS)

    Russell, A. J. B.; Mooney, M. K.; Leake, J. E.; Hudson, H. S.

    2016-01-01

    Sunquakes are the surface signatures of acoustic waves in the Sun’s interior that are produced by some but not all flares and coronal mass ejections (CMEs). This paper explores a mechanism for sunquake generation by the changes in magnetic field that occur during flares and CMEs, using MHD simulations with a semiempirical FAL-C atmosphere to demonstrate the generation of acoustic waves in the interior in response to changing magnetic tilt in the corona. We find that Alfvén–sound resonance combined with the ponderomotive force produces acoustic waves in the interior with sufficient energy to match sunquake observations when the magnetic field angle changes of the order of 10° in a region where the coronal field strength is a few hundred gauss or more. The most energetic sunquakes are produced when the coronal field is strong, while the variation of magnetic field strength with height and the timescale of the change in tilt are of secondary importance.

  9. THE CORONAL ABUNDANCE ANOMALIES OF M DWARFS

    Energy Technology Data Exchange (ETDEWEB)

    Wood, Brian E.; Laming, J. Martin [Naval Research Laboratory, Space Science Division, Washington, DC 20375 (United States); Karovska, Margarita, E-mail: brian.wood@nrl.navy.mil [Smithsonian Astrophysical Observatory, 60 Garden St., Cambridge, MA 02138 (United States)

    2012-07-01

    We analyze Chandra X-ray spectra of the M0 V+M0 V binary GJ 338. As quantified by X-ray surface flux, these are the most inactive M dwarfs ever observed with X-ray grating spectroscopy. We focus on measuring coronal abundances, in particular searching for evidence of abundance anomalies related to first ionization potential (FIP). In the solar corona and wind, low-FIP elements are overabundant, which is the so-called FIP effect. For other stars, particularly very active ones, an 'inverse FIP effect' is often observed, with low-FIP elements being underabundant. For both members of the GJ 338 binary, we find evidence for a modest inverse FIP effect, consistent with expectations from a previously reported correlation between spectral type and FIP bias. This amounts to strong evidence that all M dwarfs should exhibit the inverse FIP effect phenomenon, not just the active ones. We take the first step toward modeling the inverse FIP phenomenon in M dwarfs, building on past work that has demonstrated that MHD waves coursing through coronal loops can lead to a ponderomotive force that fractionates elements in a manner consistent with the FIP effect. We demonstrate that in certain circumstances this model can also lead to an inverse FIP effect, pointing the way to more detailed modeling of M dwarf coronal abundances in the future.

  10. The Coronal Abundance Anomalies of M Dwarfs

    Science.gov (United States)

    Wood, Brian E.; Laming, J. Martin; Karovska, Margarita

    2012-07-01

    We analyze Chandra X-ray spectra of the M0 V+M0 V binary GJ 338. As quantified by X-ray surface flux, these are the most inactive M dwarfs ever observed with X-ray grating spectroscopy. We focus on measuring coronal abundances, in particular searching for evidence of abundance anomalies related to first ionization potential (FIP). In the solar corona and wind, low-FIP elements are overabundant, which is the so-called FIP effect. For other stars, particularly very active ones, an "inverse FIP effect" is often observed, with low-FIP elements being underabundant. For both members of the GJ 338 binary, we find evidence for a modest inverse FIP effect, consistent with expectations from a previously reported correlation between spectral type and FIP bias. This amounts to strong evidence that all M dwarfs should exhibit the inverse FIP effect phenomenon, not just the active ones. We take the first step toward modeling the inverse FIP phenomenon in M dwarfs, building on past work that has demonstrated that MHD waves coursing through coronal loops can lead to a ponderomotive force that fractionates elements in a manner consistent with the FIP effect. We demonstrate that in certain circumstances this model can also lead to an inverse FIP effect, pointing the way to more detailed modeling of M dwarf coronal abundances in the future.

  11. THE CORONAL ABUNDANCE ANOMALIES OF M DWARFS

    International Nuclear Information System (INIS)

    Wood, Brian E.; Laming, J. Martin; Karovska, Margarita

    2012-01-01

    We analyze Chandra X-ray spectra of the M0 V+M0 V binary GJ 338. As quantified by X-ray surface flux, these are the most inactive M dwarfs ever observed with X-ray grating spectroscopy. We focus on measuring coronal abundances, in particular searching for evidence of abundance anomalies related to first ionization potential (FIP). In the solar corona and wind, low-FIP elements are overabundant, which is the so-called FIP effect. For other stars, particularly very active ones, an 'inverse FIP effect' is often observed, with low-FIP elements being underabundant. For both members of the GJ 338 binary, we find evidence for a modest inverse FIP effect, consistent with expectations from a previously reported correlation between spectral type and FIP bias. This amounts to strong evidence that all M dwarfs should exhibit the inverse FIP effect phenomenon, not just the active ones. We take the first step toward modeling the inverse FIP phenomenon in M dwarfs, building on past work that has demonstrated that MHD waves coursing through coronal loops can lead to a ponderomotive force that fractionates elements in a manner consistent with the FIP effect. We demonstrate that in certain circumstances this model can also lead to an inverse FIP effect, pointing the way to more detailed modeling of M dwarf coronal abundances in the future.

  12. EIT Observations of Coronal Mass Ejections

    Science.gov (United States)

    Gurman, J. B.; Fisher, Richard B. (Technical Monitor)

    2000-01-01

    Before the Solar and Heliospheric Observatory (SOHO), we had only the sketchiest of clues as to the nature and topology of coronal mass ejections (CMEs) below 1.1 - 1.2 solar radii. Occasionally, dimmings (or 'transient coronal holes') were observed in time series of soft X-ray images, but they were far less frequent than CME's. Simply by imaging the Sun frequently and continually at temperatures of 0.9 - 2.5 MK we have stumbled upon a zoo of CME phenomena in this previously obscured volume of the corona: (1) waves, (2) dimmings, and (3) a great variety of ejecta. In the three and a half years since our first observations of coronal waves associated with CME's, combined Large Angle Spectroscopic Coronagraph (LASCO) and extreme ultra-violet imaging telescope (EIT) synoptic observations have become a standard prediction tool for space weather forecasters, but our progress in actually understanding the CME phenomenon in the low corona has been somewhat slower. I will summarize the observations of waves, hot (> 0.9 MK) and cool ejecta, and some of the interpretations advanced to date. I will try to identify those phenomena, analysis of which could most benefit from the spectroscopic information available from ultraviolet coronograph spectrometer (UVCS) observations.

  13. The acceleration of electrons at a spherical coronal shock in a streamer-like coronal field

    Energy Technology Data Exchange (ETDEWEB)

    Kong, Xiangliang, E-mail: kongx@sdu.edu.cn; Chen, Yao, E-mail: yaochen@sdu.edu.cn [Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, and Institute of Space Sciences, Shandong University, Weihai, Shandong 264209 (China); Guo, Fan, E-mail: guofan.ustc@gmail.com [Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)

    2016-03-25

    We study the effect of large-scale coronal magnetic field on the electron acceleration at a spherical coronal shock using a test-particle method. The coronal field is approximated by an analytical solution with a streamer-like magnetic field featured by partially open magnetic field and a current sheet at the equator atop the closed region. It shows that the closed field plays the role of a trapping agency of shock-accelerated electrons, allowing for repetitive reflection and acceleration, therefore can greatly enhance the shock-electron acceleration efficiency. It is found that, with an ad hoc pitch-angle scattering, electron injected in the open field at the shock flank can be accelerated to high energies as well. In addition, if the shock is faster or stronger, a relatively harder electron energy spectrum and a larger maximum energy can be achieved.

  14. Análisis retrospectivo sobre la utilidad de las herramientas de valoración funcional, en las dolencias lumbares a nivel del ámbito laboral (Regional Canarias de Fremap, Año 2012

    Directory of Open Access Journals (Sweden)

    Alexander Vera Vicuña

    2014-01-01

    Full Text Available Introducción: La lumbalgia o dolor lumbar (DL, constituye uno de los síndromes que provocan más consultas en el sistema sanitario, constituyendo la causa más importante de desembolso compensatorio económico, bien sea por entidades públicas como la Seguridad Social o entidades aseguradoras laborales como las mutuas. Objetivo: Determinar la posible influencia de aplicar las herramientas de valoración funcional (Nedlumb/IBV 1.0 en el seguimiento de los procesos de baja laboral por dolor lumbar, en la disminución en el tiempo de baja por dolencias lumbares, así como el ahorro en los coste por compensación de días de baja laboral. Materiales y métodos: Se realizó un estudio retrospectivo, transversal, determinando el número total de paciente con diagnóstico de Lumbalgia en la Regional Canarias de Fremap en el año 2012, extrapolando el tiempo promedio de duración de nuestras baja por dicha dolencia en Contingencia Profesional (CP, con respecto al grupo II del estudio realizado por Asepeyo en Sant Cugat en 2009, denominando a nuestro grupo de estudio, Grupo-II Fremap (Lumbalgias sin valoración funcional, que se comparó con el grupo I de dicho estudio (Lumbalgias con valoración funcional. Se estudio la correlación entre ambos grupo y si el resultado de la valoración funcional, tiene un valor pronóstico, sobre el período restante de baja posterior, en cuanto a disminución del tiempo de baja o al coste económico de la misma. Resultado: Tras comparar nuestro grupo, Grupo II-Fremap, con el Grupo I, como si se hubiera realizado la valoración funcional con el Nedlumb/IBV 1.0 a los 50 días de la baja, los resultado evidenciaron una reducción total de 758.54 días de baja, que sí se correlacionaban con el ahorro del coste diario de compensación de baja (36.3€/día, se demostraba, que se podía haber conseguido un ahorro de 27.535€ en bajas por CP por patología lumbar en la Regional Canarias en el año 2012. Además, si tambi

  15. de estudios observacionales

    Directory of Open Access Journals (Sweden)

    Erik von Elm

    2008-01-01

    un documento de explicación y elaboración al que puede accederse libremente en los sitios web de PLoS Medicine, Annals of Internal Medicine y Epidemiology. Esperamos que la declaración STROBE contribuya a mejorar la calidad de la publicación de los estudios observacionales.

  16. Análisis retrospectivo de 23 años de necrólisis epidérmica tóxica en la Unidad de Quemados de Alicante, España

    Directory of Open Access Journals (Sweden)

    F.I. Castillo-Muñoz

    2014-09-01

    Full Text Available El Síndrome de Lyell o Necrólisis Epidérmica Tóxica (NET se encuadra dentro del espectro de reacciones cutáneas adversas graves y se caracteriza por presentar una baja incidencia pero una elevada mortalidad. La mayoría de los casos de NET se relacionan con una reacción medicamentosa idiosincrática. El objetivo de este trabajo es reflejar la experiencia clínica con esta entidad en la Unidad de Quemados del Hospital General Universitario de Alicante, España, durante los últimos 23 años. Realizamos un estudio retrospectivo recogiendo los datos epidemiológicos, agentes causales probables, pruebas complementarias, patologías concomitantes, tratamiento y evolución clínica. En total recogimos 16 pacientes con una media de edad de 53,19 años, 68,75% mujeres y 31,25% varones. Los antibióticos fueron los fármacos más comúnmente implicados (31,25%, seguidos de los AINES (25%. Durante el ingreso hospitalario, el 43,75% de los pacientes recibió corticoides sistémicos, el 37,5% exclusivamente tratamiento de soporte y el 25% inmunoglobulinas intravenosas. El 56,25% sufrió algún tipo de secuela, siendo la afectación ocular la más frecuente (18,75%. Calculamos el SCORTEN (Severity of illness score for toxic epidermal necrolisys para todos los pacientes en las primeras 24 horas de ingreso, siendo la suma de las probabilidades predichas de morir por NET de un 32%, cifra superior a los datos reales (mortalidad del 25%. La utilización de corticoides sistémicos sigue siendo controvertida, apareciendo en nuestro estudio un mayor número de infecciones y una mayor mortalidad asociada a dicho tratamiento. La retirada inmediata del fármaco sospechoso, el ingreso precoz en una Unidad de Quemados o de Cuidados Intensivos, el tratamiento de soporte y la reposición hidroelectrolítica, siguen siendo medidas cruciales y de primera línea en el tratamiento de estos pacientes. A pesar de que están descritos diferentes tipos de tratamiento

  17. Density Fluctuations in a Polar Coronal Hole

    Science.gov (United States)

    Hahn, Michael; D’Huys, Elke; Savin, Daniel Wolf

    2018-06-01

    We have measured the root-mean-square (rms) amplitude of intensity fluctuations, ΔI, in plume and interplume regions of a polar coronal hole. These intensity fluctuations correspond to density fluctuations. Using data from the Sun Watcher using the Active Pixel System detector and Image Processing on the Project for Onboard Autonomy (Proba2), our results extend up to a height of about 1.35 R ⊙. One advantage of the rms analysis is that it does not rely on a detailed evaluation of the power spectrum, which is limited by noise levels to low heights in the corona. The rms approach can be performed up to larger heights where the noise level is greater, provided that the noise itself can be quantified. At low heights, both the absolute ΔI, and the amplitude relative to the mean intensity, ΔI/I, decrease with height. However, starting at about 1.2 R ⊙, ΔI/I increases, reaching 20%–40% by 1.35 R ⊙. This corresponds to density fluctuations of Δn e/n e ≈ 10%–20%. The increasing relative amplitude implies that the density fluctuations are generated in the corona itself. One possibility is that the density fluctuations are generated by an instability of Alfvén waves. This generation mechanism is consistent with some theoretical models and with observations of Alfvén wave amplitudes in coronal holes. Although we find that the energy of the observed density fluctuations is small, these fluctuations are likely to play an important indirect role in coronal heating by promoting the reflection of Alfvén waves and driving turbulence.

  18. Coronal Loops: Evolving Beyond the Isothermal Approximation

    Science.gov (United States)

    Schmelz, J. T.; Cirtain, J. W.; Allen, J. D.

    2002-05-01

    Are coronal loops isothermal? A controversy over this question has arisen recently because different investigators using different techniques have obtained very different answers. Analysis of SOHO-EIT and TRACE data using narrowband filter ratios to obtain temperature maps has produced several key publications that suggest that coronal loops may be isothermal. We have constructed a multi-thermal distribution for several pixels along a relatively isolated coronal loop on the southwest limb of the solar disk using spectral line data from SOHO-CDS taken on 1998 Apr 20. These distributions are clearly inconsistent with isothermal plasma along either the line of sight or the length of the loop, and suggested rather that the temperature increases from the footpoints to the loop top. We speculated originally that these differences could be attributed to pixel size -- CDS pixels are larger, and more `contaminating' material would be expected along the line of sight. To test this idea, we used CDS iron line ratios from our data set to mimic the isothermal results from the narrowband filter instruments. These ratios indicated that the temperature gradient along the loop was flat, despite the fact that a more complete analysis of the same data showed this result to be false! The CDS pixel size was not the cause of the discrepancy; rather, the problem lies with the isothermal approximation used in EIT and TRACE analysis. These results should serve as a strong warning to anyone using this simplistic method to obtain temperature. This warning is echoed on the EIT web page: ``Danger! Enter at your own risk!'' In other words, values for temperature may be found, but they may have nothing to do with physical reality. Solar physics research at the University of Memphis is supported by NASA grant NAG5-9783. This research was funded in part by the NASA/TRACE MODA grant for Montana State University.

  19. A multi-channel coronal spectrophotometer.

    Science.gov (United States)

    Landman, D. A.; Orrall, F. Q.; Zane, R.

    1973-01-01

    We describe a new multi-channel coronal spectrophotometer system, presently being installed at Mees Solar Observatory, Mount Haleakala, Maui. The apparatus is designed to record and interpret intensities from many sections of the visible and near-visible spectral regions simultaneously, with relatively high spatial and temporal resolution. The detector, a thermoelectrically cooled silicon vidicon camera tube, has its central target area divided into a rectangular array of about 100,000 pixels and is read out in a slow-scan (about 2 sec/frame) mode. Instrument functioning is entirely under PDP 11/45 computer control, and interfacing is via the CAMAC system.

  20. Evolution of coronal and interplanetary magnetic fields

    International Nuclear Information System (INIS)

    Levine, R.H.

    1980-01-01

    Numerous studies have provided the detailed information necessary for a substantive synthesis of the empirical relation between the magnetic field of the sun and the structure of the interplanetary field. The author points out the latest techniques and studies of the global solar magnetic field and its relation to the interplanetary field. The potential to overcome most of the limitations of present methods of analysis exists in techniques of modelling the coronal magnetic field using observed solar data. Such empirical models are, in principle, capable of establishing the connection between a given heliospheric point and its magnetically-connected photospheric point, as well as the physical basis for the connection. (Auth.)

  1. Solar radio bursts of spectral type II, coronal shocks, and optical coronal transients

    Science.gov (United States)

    Maxwell, A.; Dryer, M.

    1981-01-01

    An examination is presented of the association of solar radio bursts of spectral type II and coronal shocks with solar flare ejecta observed in H-alpha, the green coronal line, and white-light coronagraphs. It is suggested that fast-moving optical coronal transients should for the most part be identified with piston-type phenomena well behind the outward-traveling shock waves that generate type II radio bursts. A general model is presented which relates type II radio bursts and coronal shocks to optically observed ejecta and consists of three main velocity regimes: (1) a quasi-hemispherical shock wave moving outward from the flare at speeds of 1000-2000 km/sec and Alfven Mach number of about 1.5; (2) the velocity of the piston driving the shock, on the order of 0.8 that of the shock; and (3) the regime of the slower-moving H-alpha ejecta, with velocities of 300-500 km/sec.

  2. Evaluation of the Minifilament-Eruption Scenario for Solar Coronal Jets in Polar Coronal Holes

    Science.gov (United States)

    Baikie, Tomi K.; Sterling, Alphonse C.; Falconer, David; Moore, Ronald L.; Savage, Sabrina L.

    2016-01-01

    Solar coronal jets are suspected to result from magnetic reconnection low in the Sun's atmosphere. Sterling et al. (2015) looked as 20 jets in polar coronal holes, using X-ray images from the Hinode/X-Ray Telescope (XRT) and EUV images from the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA). They suggested that each jet was driven by the eruption of twisted closed magnetic field carrying a small-scale filament, which they call a 'minifilament', and that the jet was produced by reconnection of the erupting field with surrounding open field. In this study, we carry out a more extensive examination of polar coronal jets. From 180 hours of XRT polar coronal hole observations spread over two years (2014-2016), we identified 130 clearly-identifiable X-ray jet events and thus determined an event rate of over 17 jets per day per in the Hinode/XRT field of view. From the broader set, we selected 25 of the largest and brightest events for further study in AIA 171, 193, 211, and 304 Angstrom images. We find that at least the majority of the jets follow the minifilament-eruption scenario, although for some cases the evolution of the minifilament in the onset of its eruption is more complex than presented in the simplified schematic of Sterling et al. (2015). For all cases in which we could make a clear determination, the spire of the X-ray jet drifted laterally away from the jet-base-edge bright point; this spire drift away from the bright point is consistent with expectations of the minifilament-eruption scenario for coronal-jet production. This work was supported with funding from the NASA/MSFC Hinode Project Office, and from the NASA HGI program.

  3. ESTUDO RETROSPECTIVO DA BRUCELOSE BOVINA NA MICRORREGIÃO DE PAU DOS FERROS, ESTADO DO RIO GRANDE DO NORTE, BRASIL

    Directory of Open Access Journals (Sweden)

    Francisco Ariclenes Olinto

    2013-03-01

    Full Text Available A brucelose bovina é uma doença bacteriana causada pela Brucella abortus, como também é uma zoonose e enfermidade infecto-contagiosa de importância econômica e em saúde pública, estando presente na lista da Organização Mundial de Saúde Animal (OIE, sendo de notificação obrigatória. Com o objetivo de avaliar essa enfermidade na Microrregião de Pau dos Ferros, Estado do Rio Grande do Norte, foi realizado um Estudo Retrospectivo compreendendo os municípios de Alexandria, Antonio Martins, Encanto, José da Penha, Major Sales, Marcelino Vieira, Paraná, Pilões, Riacho de Santana e Tenente Ananias. Analisando os dados dos relatórios mensais de exames realizados por médicos veterinários habilitados pelo Ministério da Agricultura, Pecuária e Abastecimento (MAPA, no que diz respeito ao Programa Nacional de Controle e Erradicação da Brucelose e Tuberculose Animal (PNCEBT. Foram analisados os resultados dos exames de brucelose bovina de 1077 animais de 189 propriedades, destas, quatro apresentaram animais positivos (2,12%, realizados durante o período de janeiro de 2008 a dezembro de 2009.

  4. Neoplasias malignas de glândulas salivares: estudo retrospectivo = Malignant neoplasms of salivary glands: retrospective study

    Directory of Open Access Journals (Sweden)

    Barbosa, Renata Pereira de Sousa et al.

    2005-01-01

    Full Text Available Este trabalho objetivou identificar a ocorrência de neoplasias malignas em glândulas salivares de pacientes dos hospitais de referência no tratamento de Câncer do Estado da Paraíba no período de 1998 a 2003. Foi realizado um estudo retrospectivo pelo método indireto, através da análise de 914 prontuários arquivados do Hospital Dr. Napoleão Laureano, em João Pessoa-PB, e do Centro de Cancerologia Ulisses Pinto, em Campina Grande-PB. Encontrou-se 29 casos de neoplasias malignas de glândulas salivares, dos quais 53,6% acometeram indivíduos do gênero masculino e 46,4% do feminino; a faixa etária com maior número de casos foi de 61-80 anos com 48,3%. A glândula parótida apresentou maior prevalência com 48,3%, sendo o tipo neoplásico com maior representação da amostra o Carcinoma adenóide cístico com 58,6%

  5. Extreme ultraviolet observations of coronal holes. II

    International Nuclear Information System (INIS)

    Bohlin, J.D.; Sheeley, N.R. Jr.

    1978-01-01

    Extreme-ultraviolet Skylab and ground-based solar magnetic field data have been combined to study the origin and evolution of coronal holes. It is shown that holes exist only within the large-scale unipolar magnetic cells into which the solar surface is divided at any given time. A well-defined boundary zone usually exists between the edge of a hole and the neutral line which marks the edge of its magnetic cell. This boundary zone is the region across which a cell is connected by magnetic arcades with adjacent cells of opposite polarity. Three pieces of observational evidence are offered to support the hypothesis that the magnetic lines of force from a hole are open. Kitt Peak magnetograms are used to show that, at least on a relative scale, the average field strengths within holes are quite variable, but indistinguishable from the field strengths in other quiet parts of the Sun's surface. Finally it is shown that the large, equatorial holes characteristic of the declining phase of the last solar cycle during Skylab (1973-74) were all formed as a result of the mergence of bipolar magnetic regions (BMR's), confirming an earlier hypothesis by Timothy et al. (1975). Systematic application of this model to the different aspects of the solar cycle correctly predicts the occurrence of both large, equatorial coronal holes (the 'M-regions' which cause recurrent geomagnetic storms) and the polar cap holes. (Auth.)

  6. Plasma Evolution within an Erupting Coronal Cavity

    Science.gov (United States)

    Long, David M.; Harra, Louise K.; Matthews, Sarah A.; Warren, Harry P.; Lee, Kyoung-Sun; Doschek, George A.; Hara, Hirohisa; Jenkins, Jack M.

    2018-03-01

    Coronal cavities have previously been observed to be associated with long-lived quiescent filaments and are thought to correspond to the associated magnetic flux rope. Although the standard flare model predicts a coronal cavity corresponding to the erupting flux rope, these have only been observed using broadband imaging data, restricting an analysis to the plane-of-sky. We present a unique set of spectroscopic observations of an active region filament seen erupting at the solar limb in the extreme ultraviolet. The cavity erupted and expanded rapidly, with the change in rise phase contemporaneous with an increase in nonthermal electron energy flux of the associated flare. Hot and cool filamentary material was observed to rise with the erupting flux rope, disappearing suddenly as the cavity appeared. Although strongly blueshifted plasma continued to be observed flowing from the apex of the erupting flux rope, this outflow soon ceased. These results indicate that the sudden injection of energy from the flare beneath forced the rapid eruption and expansion of the flux rope, driving strong plasma flows, which resulted in the eruption of an under-dense filamentary flux rope.

  7. BAYESIAN MAGNETOHYDRODYNAMIC SEISMOLOGY OF CORONAL LOOPS

    International Nuclear Information System (INIS)

    Arregui, I.; Asensio Ramos, A.

    2011-01-01

    We perform a Bayesian parameter inference in the context of resonantly damped transverse coronal loop oscillations. The forward problem is solved in terms of parametric results for kink waves in one-dimensional flux tubes in the thin tube and thin boundary approximations. For the inverse problem, we adopt a Bayesian approach to infer the most probable values of the relevant parameters, for given observed periods and damping times, and to extract their confidence levels. The posterior probability distribution functions are obtained by means of Markov Chain Monte Carlo simulations, incorporating observed uncertainties in a consistent manner. We find well-localized solutions in the posterior probability distribution functions for two of the three parameters of interest, namely the Alfven travel time and the transverse inhomogeneity length scale. The obtained estimates for the Alfven travel time are consistent with previous inversion results, but the method enables us to additionally constrain the transverse inhomogeneity length scale and to estimate real error bars for each parameter. When observational estimates for the density contrast are used, the method enables us to fully constrain the three parameters of interest. These results can serve to improve our current estimates of unknown physical parameters in coronal loops and to test the assumed theoretical model.

  8. Mid-term periodicities and heliospheric modulation of coronal index ...

    Indian Academy of Sciences (India)

    PRITHVI RAJ SINGH

    2018-03-06

    Mar 6, 2018 ... long-term periodicity of ∼11 years, with different solar activities. The physical processes that occur inside the. Sun are reflected by a periodic character in terms of coronal index of coronal emission (Fe XIV 530.3 nm) during solar activity cycles. Recently, a link between the strength of photospheric magnetic ...

  9. Estudio de validez predictiva

    OpenAIRE

    Barquero-Segura, José Antonio

    2003-01-01

    Proyecto de investigación Este documento es un informe ejecutivo de la información obtenida de los estudios sobre la validez predictiva de los parámetros de selección de estudiantes y su relación con el rendimiento académico. En él se presenta una síntesis de información más relevante obtenida en los últimos 17 años.

  10. Quality of coroner's post-mortems in a UK hospital.

    Science.gov (United States)

    Al Mahdy, Husayn

    2014-01-01

    The aim of this paper was, principally, to look at the coroner's post-mortem report quality regarding adult medical patients admitted to an English hospital; and to compare results with Royal College of Pathologists guidelines. Hospital clinical notes of adult medical patients dying in 2011 and who were referred to the coroner's office to determine the cause of death were scrutinised. Their clinical care was also reviewed. There needs to be a comprehensive approach to coroner's post-mortems such as routinely taking histological and microbiological specimens. Acute adult medical patient care needs to improve. Steps should be taken to ensure that comprehensive coroner's post-mortems are performed throughout the UK, including with routine histological and microbiological specimens examination. Additionally, closer collaboration between clinicians and pathologists needs to occur to improve emergency adult medical patient clinical care. The study highlights inadequacies in coroner's pathology services.

  11. Assessment of Coronal Radiographic Parameters of the Spine in the Treatment of Adolescent Idiopathic Scoliosis

    Directory of Open Access Journals (Sweden)

    Mohsen Karami

    2016-10-01

    Preoperative coronal balance is very important to make a balanced spine after surgery. Other parameters like Lenke classification or main thoracic overcorrection did not affect postoperative coronal decompensation.

  12. Factores de riesgo asociados a la mortalidad por hemorragia digestiva alta en pacientes de un hospital público: Estudio caso control

    OpenAIRE

    Corzo Maldonado, Manuel Alejandro; Guzmán Rojas, Patricia; Bravo Paredes, Eduar Alban; Gallegos López, Roxana Consuelo; Huerta Mercado-Tenorio, Jorge; Surco Ochoa, Yolanda; Prochazka Zárate, Ricardo; Piscoya Rivera, Alejandro; Pinto Valdivia, José; De los Ríos Senmache, Raúl

    2013-01-01

    Objetivo: Determinar y establecer los factores de riesgo asociados a la mortalidad por hemorragia digestiva alta (HDA) a los 30 días posteriores al episodio en el Hospital Nacional Cayetano Heredia, Lima, Perú. Materiales y métodos: Se realizó un estudio observacional analítico caso-control retrospectivo con una proporción caso: control de 1:3, analizando 180 pacientes, siendo 135 los controles y 45 los casos. Se determinó por plausibilidad biológica como posibles factores de riesgo a 14 vari...

  13. Estudio poblacional sobre el estado de salud y nutrición de habitantes de la ciudad de Mérida, México

    OpenAIRE

    Barbosa-Martín, Enrique Efraín; Fajardo-Niquete, Ileana; Sosa-Valadez, Fernando; Cetina-Sánchez, Francisco; Puc-Encalada, Ivan; Vargas-Espinosa, Rafael; Jiménez-Estrada, Rebeca; Betancur-Ancona, David Abram

    2016-01-01

    Introducción: La Encuesta Nacional de Salud y Nutrición (ENSANUT) reporta el panorama actual de la epidemiología nutricional nacional y estatal en México. Sin embargo, no existen reportes nutricionales de las capitales de los estados mexicanos. El presente trabajo tuvo como objetivo evaluar el estado de salud y nutrición en habitantes de Mérida, Yucatán, México. Material y Métodos: Estudio transversal, retrospectivo y descriptivo que utilizó los lineamientos metodológicos y diagnósticos de la...

  14. Estudio de los factores relacionados con el grado de satisfacción post-reconstrucción mamaria con implantes

    OpenAIRE

    Brea García, Beatriz

    2016-01-01

    Material y métodos Se diseño un estudio retrospectivo de las reconstrucciones mamarias realizadas con implantes a 111 mujeres entre los años 1999 y 2011 en el Servicio de Cirugía Plástica, Estética y Reparadora del Complexo Hospitalario Universitario de Santiago de Compostela. Se estudiaron las posibles variables que podrían estar relacionadas con el grado de satisfacción post-reconstrucción expresado por las pacientes. Al mismo tiempo, se realizó una valoración del resultad...

  15. La mamografía y la ecografía en el estudio de la patología mamaria en el varón

    OpenAIRE

    Muñoz Carrasco, Rafaela

    2011-01-01

    Objetivo: Valorar las variables clínicas que pueden ser útiles para diferenciar patología mamaria benigna de maligna y analizar la contribución de la mamografía y la ecografía en la evaluación de la mama masculina. Material y métodos: Estudio retrospectivo que incluye todos los pacientes varones que tuvieran realizada mamografía o ecografía entre 1993 y 2006 en nuestro hospital. Se comparan las características clínicas de los pacientes con patología mamaria benigna y maligna. Los hallazgos...

  16. Fisioterapia na paralisia facial periférica: estudo retrospectivo Physical therapy in peripheral facial paralysis: retrospective study

    Directory of Open Access Journals (Sweden)

    Márcia Regina Garanhani

    2007-02-01

    Full Text Available A paralisia facial periférica requer tratamento especializado. A fisioterapia tem como objetivo restabelecer a mímica facial. O objetivo deste estudo foi descrever e analisar os resultados da fisioterapia para indivíduos com paralisia facial periférica. FORMA DE ESTUDO: Retrospectivo. MÉTODO: Foi realizado um estudo retrospectivo em um Hospital Universitário, com autorização do Serviço de Atendimento Médico e Estatístico, no período de 1999 a 2003. Os dados são apresentados em forma descritiva, com utilização de média e mediana para variáveis numéricas e freqüência para variáveis categóricas. RESULTADOS: Foram analisados 23 prontuários durante quatro anos. Foi identificado o predomínio do sexo feminino e a média de idade foi de 32,3 anos (DP±16,5; 14 casos idiopáticas e cinco traumáticas; 12, com comprometimento motor total e 11, parcial; nos 12 casos com avaliação final, sete evoluíram para recuperação parcial e cinco para total. A fisioterapia utilizada foi cinesioterapia e orientações. CONCLUSÃO: Neste estudo os indivíduos são similares a outras populações. Foram tratados com cinesioterapia, como sugerido pela literatura científica e evoluíram com recuperação.Peripheral facial paralysis requires specialized treatment. Physical therapy aims at reestablishing facial movements. The aim of this study was to describe and to analyze physical therapy results for individuals with peripheral facial paralysis. STUDY DESIGN: Retrospective study. METHOD: A retrospective study was carried out at the University Hospital, authorized by the Statistics and Medical File Services, from 1999 to 2003. Data are presented in descriptive form with mean and median values for numeric variables and frequency for categorical variables. RESULTS: Twenty-three files were analyzed during four years. Females predominated and the average age was of 32.3 years (SD±16.5; 14 idiopathic and five trauma cases; 12 with total motor

  17. A model for a stable coronal loop

    International Nuclear Information System (INIS)

    Hoven, G.V.; Chiuderi, C.; Giachetti, R.

    1977-01-01

    We present here a new plasma-physics model of a stable active-region arch which corresponds to the structure observed in the EUV. Pressure gradients are seen, so that the equilibrium magnetic field must depart from the force-free form valid in the surrounding corona. We take advantage of the data and of the approximate cylindrical symmetry to develop a modified form of the commonly assumed sheared-spiral structure. The dynamic MHD behavior of this new pressure/field model is then evaluated by the Newcomb criterion, taken from controlled-fusion physics, and the results show short-wavelength stability in a specific parameter range. Thus we demonstrate the possibility, for pressure profiles with widths of the order of the magnetic-field scale, that such arches can persist for reasonable periods. Finally, the spatial proportions and magnetic fields of a characteristic stable coronal loop are described

  18. Image-Optimized Coronal Magnetic Field Models

    Science.gov (United States)

    Jones, Shaela I.; Uritsky, Vadim; Davila, Joseph M.

    2017-01-01

    We have reported previously on a new method we are developing for using image-based information to improve global coronal magnetic field models. In that work we presented early tests of the method which proved its capability to improve global models based on flawed synoptic magnetograms, given excellent constraints on the field in the model volume. In this follow-up paper we present the results of similar tests given field constraints of a nature that could realistically be obtained from quality white-light coronagraph images of the lower corona. We pay particular attention to difficulties associated with the line-of-sight projection of features outside of the assumed coronagraph image plane, and the effect on the outcome of the optimization of errors in localization of constraints. We find that substantial improvement in the model field can be achieved with this type of constraints, even when magnetic features in the images are located outside of the image plane.

  19. Endogenous Magnetic Reconnection in Solar Coronal Loops

    Science.gov (United States)

    Asgari-Targhi, M.; Coppi, B.; Basu, B.; Fletcher, A.; Golub, L.

    2017-12-01

    We propose that a magneto-thermal reconnection process occurring in coronal loops be the source of the heating of the Solar Corona [1]. In the adopted model, magnetic reconnection is associated with electron temperature gradients, anisotropic electron temperature fluctuations and plasma current density gradients [2]. The input parameters for our theoretical model are derived from the most recent observations of the Solar Corona. In addition, the relevant (endogenous) collective modes can produce high energy particle populations. An endogenous reconnection process is defined as being driven by factors internal to the region where reconnection takes place. *Sponsored in part by the U.S. D.O.E. and the Kavli Foundation* [1] Beafume, P., Coppi, B. and Golub, L., (1992) Ap. J. 393, 396. [2] Coppi, B. and Basu, B. (2017) MIT-LNS Report HEP 17/01.

  20. Image-optimized Coronal Magnetic Field Models

    Energy Technology Data Exchange (ETDEWEB)

    Jones, Shaela I.; Uritsky, Vadim; Davila, Joseph M., E-mail: shaela.i.jones-mecholsky@nasa.gov, E-mail: shaela.i.jonesmecholsky@nasa.gov [NASA Goddard Space Flight Center, Code 670, Greenbelt, MD 20771 (United States)

    2017-08-01

    We have reported previously on a new method we are developing for using image-based information to improve global coronal magnetic field models. In that work, we presented early tests of the method, which proved its capability to improve global models based on flawed synoptic magnetograms, given excellent constraints on the field in the model volume. In this follow-up paper, we present the results of similar tests given field constraints of a nature that could realistically be obtained from quality white-light coronagraph images of the lower corona. We pay particular attention to difficulties associated with the line-of-sight projection of features outside of the assumed coronagraph image plane and the effect on the outcome of the optimization of errors in the localization of constraints. We find that substantial improvement in the model field can be achieved with these types of constraints, even when magnetic features in the images are located outside of the image plane.

  1. Characteristics of polar coronal hole jets

    Science.gov (United States)

    Chandrashekhar, K.; Bemporad, A.; Banerjee, D.; Gupta, G. R.; Teriaca, L.

    2014-01-01

    Context. High spatial- and temporal-resolution images of coronal hole regions show a dynamical environment where mass flows and jets are frequently observed. These jets are believed to be important for the coronal heating and the acceleration of the fast solar wind. Aims: We studied the dynamics of two jets seen in a polar coronal hole with a combination of imaging from EIS and XRT onboard Hinode. We observed drift motions related to the evolution and formation of these small-scale jets, which we tried to model as well. Methods: Stack plots were used to find the drift and flow speeds of the jets. A toymodel was developed by assuming that the observed jet is generated by a sequence of single reconnection events where single unresolved blobs of plasma are ejected along open field lines, then expand and fall back along the same path, following a simple ballistic motion. Results: We found observational evidence that supports the idea that polar jets are very likely produced by multiple small-scale reconnections occurring at different times in different locations. These eject plasma blobs that flow up and down with a motion very similar to a simple ballistic motion. The associated drift speed of the first jet is estimated to be ≈27 km s-1. The average outward speed of the first jet is ≈171 km s-1, well below the escape speed, hence if simple ballistic motion is considered, the plasma will not escape the Sun. The second jet was observed in the south polar coronal hole with three XRT filters, namely, C-poly, Al-poly, and Al-mesh filters. Many small-scale (≈3″-5″) fast (≈200-300 km s-1) ejections of plasma were observed on the same day; they propagated outwards. We observed that the stronger jet drifted at all altitudes along the jet with the same drift speed of ≃7 km s-1. We also observed that the bright point associated with the first jet is a part of sigmoid structure. The time of appearance of the sigmoid and that of the ejection of plasma from the bright

  2. EUV and radio spectrum of coronal holes

    Energy Technology Data Exchange (ETDEWEB)

    Chiuderi Drago, F [Osservatorio Astrofisico di Arcetri, Florence (Italy)

    1980-03-01

    From the intensity of 19 EUV lines whose formation temperature anti T ranges from 3 x 10/sup 4/ to 1.4 x 10/sup 6/, two different models of the transition region and corona for the cell-centre and the network are derived. It is shown that both these models give radio brightness temperatures systematically higher than the observed ones. An agreement with radio data can be found only with lines formed at low temperature (anti T < 8.5 x 10/sup 5/) by decreasing the coronal temperature and the emission measure. The possibility of resolving the discrepancy by using different ion abundances has also been investigated with negative results.

  3. Coronal mass ejections and large geomagnetic storms

    International Nuclear Information System (INIS)

    Gosling, J.T.; Bame, S.J.; McComas, D.J.; Phillips, J.L.

    1990-01-01

    Previous work indicates that coronal mass ejection (CME) events in the solar wind at 1 AU can be identified by the presence of a flux of counterstreaming solar wind halo electrons (above about 80 eV). Using this technique to identify CMEs in 1 AU plasma data, the authors find that most large geomagnetic storms during the interval surrounding the last solar maximum (Aug. 1978-Oct. 1982) were associated with Earth-passage of interplanetary disturbances in which the Earth encountered both a shock and the CME driving the shock. However, only about one CME in six encountered by Earth was effective in causing a large geomagnetic storm. Slow CMEs which did not interact strongly with the ambient solar wind ahead were particularly ineffective in a geomagnetic sense

  4. Determination of Coronal Magnetic Fields from Vector Magnetograms

    Science.gov (United States)

    Mikic, Zoran

    1997-01-01

    During the course of the present contract we developed an 'evolutionary technique' for the determination of force-free coronal magnetic fields from vector magnetograph observations. The method can successfully generate nonlinear force- free fields (with non-constant-a) that match vector magnetograms. We demonstrated that it is possible to determine coronal magnetic fields from photospheric measurements, and we applied it to vector magnetograms of active regions. We have also studied theoretical models of coronal fields that lead to disruptions. Specifically, we have demonstrated that the determination of force-free fields from exact boundary data is a well-posed mathematical problem, by verifying that the computed coronal field agrees with an analytic force-free field when boundary data for the analytic field are used; demonstrated that it is possible to determine active-region coronal magnetic fields from photospheric measurements, by computing the coronal field above active region 5747 on 20 October 1989, AR6919 on 15 November 1991, and AR7260 on 18 August 1992, from data taken with the Stokes Polarimeter at Mees Solar Observatory, University of Hawaii; started to analyze active region 7201 on 19 June 1992 using measurements made with the Advanced Stokes Polarimeter at NSO/Sac Peak; investigated the effects of imperfections in the photospheric data on the computed coronal magnetic field; documented the coronal field structure of AR5747 and compared it to the morphology of footpoint emission in a flare, showing that the 'high- pressure' H-alpha footpoints are connected by coronal field lines; shown that the variation of magnetic field strength along current-carrying field lines is significantly different from the variation in a potential field, and that the resulting near-constant area of elementary flux tubes is consistent with observations; begun to develop realistic models of coronal fields which can be used to study flare trigger mechanisms; demonstrated that

  5. PROMINENCE ACTIVATION BY CORONAL FAST MODE SHOCK

    Energy Technology Data Exchange (ETDEWEB)

    Takahashi, Takuya [Department of Astronomy, Kyoto University, Sakyo, Kyoto, 606-8502 (Japan); Asai, Ayumi [Unit of Synergetic Studies for Space, Kyoto University, Yamashina, Kyoto 607-8471 (Japan); Shibata, Kazunari, E-mail: takahashi@kwasan.kyoto-u.ac.jp [Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471 (Japan)

    2015-03-01

    An X5.4 class flare occurred in active region NOAA11429 on 2012 March 7. The flare was associated with a very fast coronal mass ejection (CME) with a velocity of over 2500 km s{sup −1}. In the images taken with the Solar Terrestrial Relations Observatory-B/COR1, a dome-like disturbance was seen to detach from an expanding CME bubble and propagated further. A Type-II radio burst was also observed at the same time. On the other hand, in extreme ultraviolet images obtained by the Solar Dynamic Observatory/Atmospheric Imaging Assembly (AIA), the expanding dome-like structure and its footprint propagating to the north were observed. The footprint propagated with an average speed of about 670 km s{sup −1} and hit a prominence located at the north pole and activated it. During the activation, the prominence was strongly brightened. On the basis of some observational evidence, we concluded that the footprint in AIA images and the ones in COR1 images are the same, that is, the MHD fast mode shock front. With the help of a linear theory, the fast mode Mach number of the coronal shock is estimated to be between 1.11 and 1.29 using the initial velocity of the activated prominence. Also, the plasma compression ratio of the shock is enhanced to be between 1.18 and 2.11 in the prominence material, which we consider to be the reason for the strong brightening of the activated prominence. The applicability of linear theory to the shock problem is tested with a nonlinear MHD simulation.

  6. Measurements of EUV coronal holes and open magnetic flux

    International Nuclear Information System (INIS)

    Lowder, C.; Qiu, J.; Leamon, R.; Liu, Y.

    2014-01-01

    Coronal holes are regions on the Sun's surface that map the footprints of open magnetic field lines. We have developed an automated routine to detect and track boundaries of long-lived coronal holes using full-disk extreme-ultraviolet (EUV) images obtained by SOHO/EIT, SDO/AIA, and STEREO/EUVI. We measure coronal hole areas and magnetic flux in these holes, and compare the measurements with calculations by the potential field source surface (PFSS) model. It is shown that, from 1996 through 2010, the total area of coronal holes measured with EIT images varies between 5% and 17% of the total solar surface area, and the total unsigned open flux varies between (2-5)× 10 22 Mx. The solar cycle dependence of these measurements is similar to the PFSS results, but the model yields larger hole areas and greater open flux than observed by EIT. The AIA/EUVI measurements from 2010-2013 show coronal hole area coverage of 5%-10% of the total surface area, with significant contribution from low latitudes, which is under-represented by EIT. AIA/EUVI have measured much enhanced open magnetic flux in the range of (2-4)× 10 22 Mx, which is about twice the flux measured by EIT, and matches with the PFSS calculated open flux, with discrepancies in the location and strength of coronal holes. A detailed comparison between the three measurements (by EIT, AIA-EUVI, and PFSS) indicates that coronal holes in low latitudes contribute significantly to the total open magnetic flux. These low-latitude coronal holes are not well measured with either the He I 10830 line in previous studies, or EIT EUV images; neither are they well captured by the static PFSS model. The enhanced observations from AIA/EUVI allow a more accurate measure of these low-latitude coronal holes and their contribution to open magnetic flux.

  7. Measurements of EUV coronal holes and open magnetic flux

    Energy Technology Data Exchange (ETDEWEB)

    Lowder, C.; Qiu, J.; Leamon, R. [Department of Physics, Montana State University, Bozeman, MT 59717 (United States); Liu, Y., E-mail: clowder@solar.physics.montana.edu [W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305 (United States)

    2014-03-10

    Coronal holes are regions on the Sun's surface that map the footprints of open magnetic field lines. We have developed an automated routine to detect and track boundaries of long-lived coronal holes using full-disk extreme-ultraviolet (EUV) images obtained by SOHO/EIT, SDO/AIA, and STEREO/EUVI. We measure coronal hole areas and magnetic flux in these holes, and compare the measurements with calculations by the potential field source surface (PFSS) model. It is shown that, from 1996 through 2010, the total area of coronal holes measured with EIT images varies between 5% and 17% of the total solar surface area, and the total unsigned open flux varies between (2-5)× 10{sup 22} Mx. The solar cycle dependence of these measurements is similar to the PFSS results, but the model yields larger hole areas and greater open flux than observed by EIT. The AIA/EUVI measurements from 2010-2013 show coronal hole area coverage of 5%-10% of the total surface area, with significant contribution from low latitudes, which is under-represented by EIT. AIA/EUVI have measured much enhanced open magnetic flux in the range of (2-4)× 10{sup 22} Mx, which is about twice the flux measured by EIT, and matches with the PFSS calculated open flux, with discrepancies in the location and strength of coronal holes. A detailed comparison between the three measurements (by EIT, AIA-EUVI, and PFSS) indicates that coronal holes in low latitudes contribute significantly to the total open magnetic flux. These low-latitude coronal holes are not well measured with either the He I 10830 line in previous studies, or EIT EUV images; neither are they well captured by the static PFSS model. The enhanced observations from AIA/EUVI allow a more accurate measure of these low-latitude coronal holes and their contribution to open magnetic flux.

  8. Case report: pre-eruptive intra-coronal radiolucencies revisited.

    LENUS (Irish Health Repository)

    Counihan, K P

    2012-08-01

    Pre-eruptive intra-coronal radiolucency (PEIR) describes a radiolucent lesion located in the coronal dentine, just beneath the enamel-dentine junction of unerupted teeth. The prevalence of this lesion varies depending on the type and quality of radiographic exposure and age of patients used for assessment. The aetiology of pre-eruptive intra-coronal radiolucent lesions is not fully understood, but published clinical and histological evidence suggest that these lesions are resorptive in nature. Issues around the diagnosis, treatment planning and clinical management of this lesion are explored using previously unreported cases.

  9. un estudio comparativo

    Directory of Open Access Journals (Sweden)

    Federico Varona

    2007-01-01

    Full Text Available La comunicación efectiva es uno de los mayores retos que tienen hoy las organizaciones y empresas tanto a nivel nacional como internacional (global. Este artículo presenta los resultados de la investigación realizada por un equipo internacional de investigadores interesados en descubrir y comparar las conductas comunicativas o estilos de comunicación de los empleados finlandeses y mexicanos cuando interactúan con sus superiores. Para ello presentamos: primero, un breve marco teórico del estudio; segundo, la metodología; tercero, los resultados del análisis estadístico comparativo entre los empleados de Finlandia y México; cuarto, las conclusiones generales y su explicación cultural; y quinto, las implicaciones teóricas y prácticas de este estudio con respecto a las competencias comunicativas necesarias para la comunicación efectiva entre empleados y superiores tanto en organizaciones nacionales como internacionales (globales.

  10. Tuberculose infantil: estudo retrospectivo

    Directory of Open Access Journals (Sweden)

    Boaventura Antonio dos Santos

    2011-10-01

    Full Text Available Introdução: A tuberculose (TB infantil permanece como uma das doenças mais prevalentes e preocupantes no mundo, sobretudo em nações em desenvolvimento, onde as taxas são ainda mais elevadas e os casos descritos subestimados pela dificuldade em se estabelecer um diagnóstico definitivo. Dessa forma, este estudo tem como objetivo descrever o perfil clínico e epidemiológico dos pacientes com TB infantil pulmonar e extrapulmonar. Métodos: Foram avaliados retrospectivamente, através de questionário, pacientes com idade de até 15 anos, internados no Serviço de Pediatria do HCPA, no período de janeiro de 2002 a setembro de 2007.   Resultados: Dos 52 pacientes incluídos, 63% apresentavam TB pulmonar. Das formas extra-pulmonares, a meningoencefalite foi a mais prevalente (22%. Comorbidades foram dectadas em 31 (60% pacientes, dos quais 15 (29% apresentavam desnutrição grave, 9 (18% HIV positivo e 7 (13% pneumopatia crônica. Das manifestações clínicas, febre e tosse estavam presentes na maioria dos pacientes. O padrão radiológico predominante foi o de consolidação pulmonar (51%. A maioria dos pacientes referia história de contato com paciente bacilífero (64%. Conclusão: A TB pulmonar representa a principal forma de apresentação clínica da TB, sendo o diagnóstico feito de forma presuntiva na maioria dos casos. O diagnóstico baseado na comprovação bacteriológica foi obtido numa minoria de pacientes, demonstrando a importância dos achados clínico-laboratoriais, história epidemiológica e vacinal para o diagnóstico. Nesse sentido, a criação de escores tem se tornado uma ferramenta de fácil acesso e com razoável acurácia para auxiliar o diagnóstico de TB em serviços de baixa complexidade, especialmente o ambulatorial.

  11. Fast Breakdown as Coronal/Ionization Waves?

    Science.gov (United States)

    Krehbiel, P. R.; Petersen, D.; da Silva, C. L.

    2017-12-01

    Studies of high-power narrow bipolar events (NBEs) have shown they are produced by a newly-recognized breakdown process called fast positive breakdown (FPB, Rison et al., 2016, doi:10.1038/ncomms10721). The breakdown was inferred to be produced by a system of positive streamers that propagate at high speed ( ˜3-6 x 107 m/s) due to occurring in a localized region of strong electric field. The polarity of the breakdown was determined from broadband interferometer (INTF) observations of the propagation direction of its VHF radiation, which was downward into the main negative charge region of a normally-electrified storm. Subsequent INTF observations being conducted in at Kennedy Space Center in Florida have shown a much greater incidence of NBEs than in New Mexico. Among the larger dataset have been clear-cut instances of some NBEs being produced by upward breakdown that would be of negative polarity. The speed and behavior of the negative breakdown is the same as that of the fast positive, leading to it being termed fast negative breakdown (FNB). The similarity (not too mention its occurrence) is surprising, given the fact that negative streamers and breakdown develops much differently than that of positive breakdown. The question is how this happens. In this study, we compare fast breakdown characteristics to well-known streamer properties as inferred from laboratory experiments and theoretical analysis. Additionally, we begin to explore the possibility that both polarities of fast breakdown are produced by what may be called coronal or ionization waves, in which the enhanced electric field produced by streamer or coronal breakdown of either polarity propagates away from the advancing front at the speed of light into a medium that is in a metastable condition of being at the threshold of hydrometeor-mediated corona onset or other ionization processes. The wave would develop at a faster speed than the streamer breakdown that gives rise to it, and thus would be

  12. LONG-TERM TREND OF SOLAR CORONAL HOLE DISTRIBUTION FROM 1975 TO 2014

    Energy Technology Data Exchange (ETDEWEB)

    Fujiki, K.; Tokumaru, M.; Hayashi, K.; Satonaka, D. [Institute for Space-Earth Environmental Research (ISEE), Nagoya University, Furo-cho, Chikusa, Nagoya Aichi 464-8601 (Japan); Hakamada, K., E-mail: fujiki@isee.nagoya-u.ac.jp [Department of Natural Science and Mathematics, Chubu University, 1200 Matsumoto-cho, Kasugai, Aichi 487-8501 (Japan)

    2016-08-20

    We developed an automated prediction technique for coronal holes using potential magnetic field extrapolation in the solar corona to construct a database of coronal holes appearing from 1975 February to 2015 July (Carrington rotations from 1625 to 2165). Coronal holes are labeled with the location, size, and average magnetic field of each coronal hole on the photosphere and source surface. As a result, we identified 3335 coronal holes and found that the long-term distribution of coronal holes shows a similar pattern known as the magnetic butterfly diagram, and polar/low-latitude coronal holes tend to decrease/increase in the last solar minimum relative to the previous two minima.

  13. Coronal Magnetic Field Lines and Electrons Associated with Type III

    Indian Academy of Sciences (India)

    Coronal Magnetic Field Lines and Electrons Associated with Type III–V Radio Bursts in a Solar Flare ... velocities of the electron streams associated with the above two types of bursts indicate ... Journal of Astrophysics and Astronomy | News ...

  14. Coroner Autopsy Findings Among Children and Adolescents of ...

    African Journals Online (AJOL)

    year retrospective study of coroner autopsies carried out on children I adolescents aged between 0-19 years, evaluated the pattern, causes and demographic features of childhood deaths in Rivers state, Nigeria. Methods A retrospective remew of ...

  15. Energy released by the interaction of coronal magnetic fields

    International Nuclear Information System (INIS)

    Sheeley, N.R. Jr.

    1976-01-01

    Comparisons between coronal spectroheliograms and photospheric magnetograms are presented to support the idea that as coronal magnetic fields interact, a process of field line reconnection usually takes place as a natural way of preventing magnetic stresses from building up in the lower corona. This suggests that the energy which would have been stored in stressed fields in continuously released as kinetic energy of material being driven aside to make way for the reconnecting fields. However, this kinetic energy is negligible compared to the thermal energy of the coronal plasma. Therefore, it appears that these slow adjustments of coronal magnetic fields cannot account for even the normal heating of the corona, much less the energetic events associated with solar flares. (Auth.)

  16. The X-ray signature of solar coronal mass

    Science.gov (United States)

    Harrison, R. A.; Waggett, P. W.; Bentley, R. D.; Phillips, K. J. H.; Bruner, M.

    1985-01-01

    The coronal response to six solar X-ray flares has been investigated. At a time coincident with the projected onset of the white-light coronal mass ejection associated with each flare, there is a small, discrete soft X-ray enhancement. These enhancements (precursors) precede by typically about 20 m the impulsive phase of the solar flare which is dominant by the time the coronal mass ejection has reached an altitude above 0.5 solar radii. Motions of hot X-ray emitting plasma, during the precursors, which may well be a signature of the mass ejection onsets, are identified. Further investigations have also revealed a second class of X-ray coronal transient, during the main phase of the flare. These appear to be associated with magnetic reconnection above post-flare loop systems.

  17. Cyclical Variation of the Quiet Corona and Coronal Holes

    Indian Academy of Sciences (India)

    tribpo

    Key words. Coronagraphs—solar activity cycle—solar corona—total ... can be divided into the quiet sun (including coronal holes) and active regions. The ... regions has attracted attention and is termed as 'the extended solar cycle'. Here the.

  18. Coronal Structures as Tracers of Sub-Surface Processes

    Indian Academy of Sciences (India)

    tribpo

    dramatic differences in appearance and physical processes, all these structures share a common ... mena that indicate a close relationship between coronal and sub-photo- spheric processes. .... 8) maintaining the same chirality. Large scale ...

  19. The nature of micro CMEs within coronal holes

    Science.gov (United States)

    Bothmer, Volker; Nistico, Giuseppe; Zimbardo, Gaetano; Patsourakos, Spiros; Bosman, Eckhard

    Whilst investigating the origin and characteristics of coronal jets and large-scale CMEs identi-fied in data from the SECCHI (Sun Earth Connection Coronal and Heliospheric Investigation) instrument suites on board the two STEREO satellites, we discovered transient events that originated in the low corona with a morphology resembling that of typical three-part struc-tured coronal mass ejections (CMEs). However, the CMEs occurred on considerably smaller spatial scales. In this presentation we show evidence for the existence of small-scale CMEs from inside coronal holes and present quantitative estimates of their speeds and masses. We interprete the origin and evolution of micro CMEs as a natural consequence of the emergence of small-scale magnetic bipoles related to the Sun's ever changing photospheric magnetic flux on various scales and their interactions with the ambient plasma and magnetic field. The analysis of CMEs is performed within the framework of the EU Erasmus and FP7 SOTERIA projects.

  20. MHD Simulations of the Eruption of Coronal Flux Ropes under Coronal Streamers

    Energy Technology Data Exchange (ETDEWEB)

    Fan, Yuhong, E-mail: yfan@ucar.edu [High Altitude Observatory, National Center for Atmospheric Research, 3080 Center Green Drive, Boulder, CO 80301 (United States)

    2017-07-20

    Using three-dimensional magnetohydrodynamic (MHD) simulations, we investigate the eruption of coronal flux ropes underlying coronal streamers and the development of a prominence eruption. We initialize a quasi-steady solution of a coronal helmet streamer, into which we impose at the lower boundary the slow emergence of a part of a twisted magnetic torus. As a result, a quasi-equilibrium flux rope is built up under the streamer. With varying streamer sizes and different lengths and total twists of the flux rope that emerges, we found different scenarios for the evolution from quasi-equilibrium to eruption. In the cases with a broad streamer, the flux rope remains well confined until there is sufficient twist such that it first develops the kink instability and evolves through a sequence of kinked, confined states with increasing height until it eventually develops a “hernia-like” ejective eruption. For significantly twisted flux ropes, prominence condensations form in the dips of the twisted field lines due to runaway radiative cooling. Once formed, the prominence-carrying field becomes significantly non-force-free due to the weight of the prominence, despite having low plasma β . As the flux rope erupts, the prominence erupts, showing substantial draining along the legs of the erupting flux rope. The prominence may not show a kinked morphology even though the flux rope becomes kinked. On the other hand, in the case with a narrow streamer, the flux rope with less than one wind of twist can erupt via the onset of the torus instability.

  1. Dos estudios de casos

    Directory of Open Access Journals (Sweden)

    Hernán Guillermo Salazar Morales

    1989-04-01

    Full Text Available RESUMEN A continuación se presenta dos casos de estudio en donde se puede apreciar a la forma  como se establecen  las relaciones en una organización y lo que una DECISION  puede llegar a incidir en el desarrollo de las operaciones de una empresa. Decisiones basadas en la intuición, o en corazonadas, frecuentemente conducen en dirección equivocada, ocasionando pérdidas en tiempo, personal y dinero. El proceso de toma de decisiones deben ser TAREAS ESTRUCTURADAS que se sustenten con hechos. Su ejecución debe hacerse secuencialmente y cumplir con cada uno de sus pasos. El diseño de los  casos está orientado para que  sirvan como material de aplicación en la asignatura de  taller de planeación.

  2. DE AGUA. ESTUDIO PRELIMINAR

    Directory of Open Access Journals (Sweden)

    Esther E. Pellizzari

    2015-01-01

    Full Text Available El objetivo del presente estudio fue investigar la resistencia al arsénico en cultivos puros de Pseudomonas aeruginosa , aislada de aguas subterráneas de Presidencia Roque Sáenz Peña, provincia de Chaco y evaluar la posibilidad de su uso para la remoción de este contaminante presente en las aguas subterráneas. Las cepas fueron inmovilizadas en piedra natural y se cu ltivaron en caldo de sales y 1 mgAs/L . Se observó la resistencia al arsénico y la formación de biofilm , logrando la interacción entre la s células, roca y arsénico . L a remoción de arsénico se evaluó durante 3 meses y el porcentaje de eliminación de arsénico al final del experimento fue 60%.

  3. THE CONTRIBUTION OF CORONAL JETS TO THE SOLAR WIND

    Energy Technology Data Exchange (ETDEWEB)

    Lionello, R.; Török, T.; Titov, V. S.; Mikić, Z.; Linker, J. A. [Predictive Science Inc., 9990 Mesa Rim Road, Suite 170, San Diego, CA 92121 (United States); Leake, J. E.; Linton, M. G., E-mail: lionel@predsci.com [US Naval Research Laboratory 4555 Overlook Avenue, SW Washington, DC 20375 (United States)

    2016-11-01

    Transient collimated plasma eruptions in the solar corona, commonly known as coronal (or X-ray) jets, are among the most interesting manifestations of solar activity. It has been suggested that these events contribute to the mass and energy content of the corona and solar wind, but the extent of these contributions remains uncertain. We have recently modeled the formation and evolution of coronal jets using a three-dimensional (3D) magnetohydrodynamic (MHD) code with thermodynamics in a large spherical domain that includes the solar wind. Our model is coupled to 3D MHD flux-emergence simulations, i.e., we use boundary conditions provided by such simulations to drive a time-dependent coronal evolution. The model includes parametric coronal heating, radiative losses, and thermal conduction, which enables us to simulate the dynamics and plasma properties of coronal jets in a more realistic manner than done so far. Here, we employ these simulations to calculate the amount of mass and energy transported by coronal jets into the outer corona and inner heliosphere. Based on observed jet-occurrence rates, we then estimate the total contribution of coronal jets to the mass and energy content of the solar wind to (0.4–3.0)% and (0.3–1.0)%, respectively. Our results are largely consistent with the few previous rough estimates obtained from observations, supporting the conjecture that coronal jets provide only a small amount of mass and energy to the solar wind. We emphasize, however, that more advanced observations and simulations (including parametric studies) are needed to substantiate this conjecture.

  4. Calcium K-line network in coronal holes

    Energy Technology Data Exchange (ETDEWEB)

    Marsh, K A [Hale Observatories, Pasadena, Calif. (USA)

    1977-05-01

    Microphotometry of calcium K-line photographs in the regions of polar coronal holes shows that the chromospheric network exterior to a hole has a slightly broader intensity distribution than that inside the hole itself, a fact which can be attributed to a greater number of bright network elements outside the hole. These bright elements presumably represent the enhanced network resulting from the dispersal of magnetic flux from old active regions, a hypothesis which is consistent with current ideas of coronal hole formation.

  5. Photospheric Driving of Non-Potential Coronal Magnetic Field Simulations

    Science.gov (United States)

    2016-09-19

    synthesize observable emission . In future, the computational speed of the MF model makes it a potential avenue for near- real time and/or ensemble...AFRL-AFOSR-UK-TR-2016-0030 PHOTOSPHERIC DRIVING OF NON-POTENTIAL CORONAL MAGNETIC FIELD SIMULATIONS Anthony Yeates UNIVERSITY OF DURHAM Final Report...Final 3. DATES COVERED (From - To)  15 Sep 2014 to 14 Sep 2017 4. TITLE AND SUBTITLE PHOTOSPHERIC DRIVING OF NON-POTENTIAL CORONAL MAGNETIC FIELD

  6. Culex coronator in coastal Georgia and South Carolina.

    Science.gov (United States)

    Moulis, Robert A; Russell, Jennifer D; Lewandowski, Henry B; Thompson, Pamela S; Heusel, Jeffrey L

    2008-12-01

    In 2007, adult Culex coronator were collected in Chatham County, Georgia, and Jasper County, South Carolina, during nuisance and disease vector surveillance efforts. A total of 75 specimens of this species were collected at 8 widely separated locations in Chatham County, Georgia, and 4 closely situated sites in Jasper County, South Carolina. These represent the first Atlantic coastal records of this species in Georgia and the first confirmed records of Cx. coronator in South Carolina.

  7. Reconstructing the Morphology of an Evolving Coronal Mass Ejection

    Science.gov (United States)

    2009-01-01

    694, 707 Wood, B. E., Howard, R. A ., Thernisien, A ., Plunkett, S. P., & Socker, D. G. 2009b, Sol. Phys., 259, 163 Wood, B. E., Karovska , M., Chen, J...Reconstructing the Morphology of an Evolving Coronal Mass Ejection B. E. Wood, R. A . Howard, D. G. Socker Naval Research Laboratory, Space Science...mission, we empirically reconstruct the time-dependent three-dimensional morphology of a coronal mass ejection (CME) from 2008 June 1, which exhibits

  8. Active Longitude and Coronal Mass Ejection Occurrences

    International Nuclear Information System (INIS)

    Gyenge, N.; Kiss, T. S.; Erdélyi, R.; Singh, T.; Srivastava, A. K.

    2017-01-01

    The spatial inhomogeneity of the distribution of coronal mass ejection (CME) occurrences in the solar atmosphere could provide a tool to estimate the longitudinal position of the most probable CME-capable active regions in the Sun. The anomaly in the longitudinal distribution of active regions themselves is often referred to as active longitude (AL). In order to reveal the connection between the AL and CME spatial occurrences, here we investigate the morphological properties of active regions. The first morphological property studied is the separateness parameter, which is able to characterize the probability of the occurrence of an energetic event, such as a solar flare or CME. The second morphological property is the sunspot tilt angle. The tilt angle of sunspot groups allows us to estimate the helicity of active regions. The increased helicity leads to a more complex buildup of the magnetic structure and also can cause CME eruption. We found that the most complex active regions appear near the AL and that the AL itself is associated with the most tilted active regions. Therefore, the number of CME occurrences is higher within the AL. The origin of the fast CMEs is also found to be associated with this region. We concluded that the source of the most probably CME-capable active regions is at the AL. By applying this method, we can potentially forecast a flare and/or CME source several Carrington rotations in advance. This finding also provides new information for solar dynamo modeling.

  9. Active Longitude and Coronal Mass Ejection Occurrences

    Energy Technology Data Exchange (ETDEWEB)

    Gyenge, N.; Kiss, T. S.; Erdélyi, R. [Solar Physics and Space Plasmas Research Centre (SP2RC), School of Mathematics and Statistics, University of Sheffield Hounsfield Road, Hicks Building, Sheffield S3 7RH (United Kingdom); Singh, T.; Srivastava, A. K., E-mail: n.g.gyenge@sheffield.ac.uk [Department of Physics, Indian Institute of Technology (Banaras Hindu University), Varanasi (India)

    2017-03-20

    The spatial inhomogeneity of the distribution of coronal mass ejection (CME) occurrences in the solar atmosphere could provide a tool to estimate the longitudinal position of the most probable CME-capable active regions in the Sun. The anomaly in the longitudinal distribution of active regions themselves is often referred to as active longitude (AL). In order to reveal the connection between the AL and CME spatial occurrences, here we investigate the morphological properties of active regions. The first morphological property studied is the separateness parameter, which is able to characterize the probability of the occurrence of an energetic event, such as a solar flare or CME. The second morphological property is the sunspot tilt angle. The tilt angle of sunspot groups allows us to estimate the helicity of active regions. The increased helicity leads to a more complex buildup of the magnetic structure and also can cause CME eruption. We found that the most complex active regions appear near the AL and that the AL itself is associated with the most tilted active regions. Therefore, the number of CME occurrences is higher within the AL. The origin of the fast CMEs is also found to be associated with this region. We concluded that the source of the most probably CME-capable active regions is at the AL. By applying this method, we can potentially forecast a flare and/or CME source several Carrington rotations in advance. This finding also provides new information for solar dynamo modeling.

  10. Active Longitude and Coronal Mass Ejection Occurrences

    Science.gov (United States)

    Gyenge, N.; Singh, T.; Kiss, T. S.; Srivastava, A. K.; Erdélyi, R.

    2017-03-01

    The spatial inhomogeneity of the distribution of coronal mass ejection (CME) occurrences in the solar atmosphere could provide a tool to estimate the longitudinal position of the most probable CME-capable active regions in the Sun. The anomaly in the longitudinal distribution of active regions themselves is often referred to as active longitude (AL). In order to reveal the connection between the AL and CME spatial occurrences, here we investigate the morphological properties of active regions. The first morphological property studied is the separateness parameter, which is able to characterize the probability of the occurrence of an energetic event, such as a solar flare or CME. The second morphological property is the sunspot tilt angle. The tilt angle of sunspot groups allows us to estimate the helicity of active regions. The increased helicity leads to a more complex buildup of the magnetic structure and also can cause CME eruption. We found that the most complex active regions appear near the AL and that the AL itself is associated with the most tilted active regions. Therefore, the number of CME occurrences is higher within the AL. The origin of the fast CMEs is also found to be associated with this region. We concluded that the source of the most probably CME-capable active regions is at the AL. By applying this method, we can potentially forecast a flare and/or CME source several Carrington rotations in advance. This finding also provides new information for solar dynamo modeling.

  11. Geometric Model of a Coronal Cavity

    Science.gov (United States)

    Kucera, Therese A.; Gibson, S. E.; Ratawicki, D.; Dove, J.; deToma, G.; Hao, J.; Hudson, H. S.; Marque, C.; McIntosh, P. S.; Reeves, K. K.; hide

    2010-01-01

    We observed a coronal cavity from August 8-18 2007 during a multi-instrument observing campaign organized under the auspices of the International Heliophysical Year (IHY). Here we present initial efforts to model the cavity with a geometrical streamer-cavity model. The model is based the white-light streamer mode] of Gibson et a]. (2003 ), which has been enhanced by the addition of a cavity and the capability to model EUV and X-ray emission. The cavity is modeled with an elliptical cross-section and Gaussian fall-off in length and width inside the streamer. Density and temperature can be varied in the streamer and cavity and constrained via comparison with data. Although this model is purely morphological, it allows for three-dimensional, multi-temperature analysis and characterization of the data, which can then provide constraints for future physical modeling. Initial comparisons to STEREO/EUVI images of the cavity and streamer show that the model can provide a good fit to the data. This work is part of the effort of the International Space Science Institute International Team on Prominence Cavities

  12. Guided flows in coronal magnetic flux tubes

    Science.gov (United States)

    Petralia, A.; Reale, F.; Testa, P.

    2018-01-01

    Context. There is evidence that coronal plasma flows break down into fragments and become laminar. Aims: We investigate this effect by modelling flows confined along magnetic channels. Methods: We consider a full magnetohydrodynamic (MHD) model of a solar atmosphere box with a dipole magnetic field. We compare the propagation of a cylindrical flow perfectly aligned with the field to that of another flow with a slight misalignment. We assume a flow speed of 200 km s-1 and an ambient magnetic field of 30 G. Results: We find that although the aligned flow maintains its cylindrical symmetry while it travels along the magnetic tube, the misaligned one is rapidly squashed on one side, becoming laminar and eventually fragmented because of the interaction and back-reaction of the magnetic field. This model could explain an observation made by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory of erupted fragments that fall back onto the solar surface as thin and elongated strands and end up in a hedge-like configuration. Conclusions: The initial alignment of plasma flow plays an important role in determining the possible laminar structure and fragmentation of flows while they travel along magnetic channels. Movies are available in electronic form at http://www.aanda.org

  13. ANATOMY OF DEPLETED INTERPLANETARY CORONAL MASS EJECTIONS

    Energy Technology Data Exchange (ETDEWEB)

    Kocher, M.; Lepri, S. T.; Landi, E.; Zhao, L.; Manchester, W. B. IV, E-mail: mkocher@umich.edu [Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109-2143 (United States)

    2017-01-10

    We report a subset of interplanetary coronal mass ejections (ICMEs) containing distinct periods of anomalous heavy-ion charge state composition and peculiar ion thermal properties measured by ACE /SWICS from 1998 to 2011. We label them “depleted ICMEs,” identified by the presence of intervals where C{sup 6+}/C{sup 5+} and O{sup 7+}/O{sup 6+} depart from the direct correlation expected after their freeze-in heights. These anomalous intervals within the depleted ICMEs are referred to as “Depletion Regions.” We find that a depleted ICME would be indistinguishable from all other ICMEs in the absence of the Depletion Region, which has the defining property of significantly low abundances of fully charged species of helium, carbon, oxygen, and nitrogen. Similar anomalies in the slow solar wind were discussed by Zhao et al. We explore two possibilities for the source of the Depletion Region associated with magnetic reconnection in the tail of a CME, using CME simulations of the evolution of two Earth-bound CMEs described by Manchester et al.

  14. A Catalog of Coronal "EIT Wave" Transients

    Science.gov (United States)

    Thompson, B. J.; Myers, D. C.

    2009-01-01

    Solar and Heliospheric Observatory (SOHO) Extreme ultraviolet Imaging Telescope (EIT) data have been visually searched for coronal "EIT wave" transients over the period beginning from 1997 March 24 and extending through 1998 June 24. The dates covered start at the beginning of regular high-cadence (more than one image every 20 minutes) observations, ending at the four-month interruption of SOHO observations in mid-1998. One hundred and seventy six events are included in this catalog. The observations range from "candidate" events, which were either weak or had insufficient data coverage, to events which were well defined and were clearly distinguishable in the data. Included in the catalog are times of the EIT images in which the events are observed, diagrams indicating the observed locations of the wave fronts and associated active regions, and the speeds of the wave fronts. The measured speeds of the wave fronts varied from less than 50 to over 700 km s(exp -1) with "typical" speeds of 200-400 km s(exp -1).

  15. A CATALOG OF CORONAL 'EIT WAVE' TRANSIENTS

    International Nuclear Information System (INIS)

    Thompson, B. J.; Myers, D. C.

    2009-01-01

    Solar and Heliospheric Observatory (SOHO) Extreme ultraviolet Imaging Telescope (EIT) data have been visually searched for coronal 'EIT wave' transients over the period beginning from 1997 March 24 and extending through 1998 June 24. The dates covered start at the beginning of regular high-cadence (more than 1 image every 20 minutes) observations, ending at the four-month interruption of SOHO observations in mid-1998. One hundred and seventy six events are included in this catalog. The observations range from 'candidate' events, which were either weak or had insufficient data coverage, to events which were well defined and were clearly distinguishable in the data. Included in the catalog are times of the EIT images in which the events are observed, diagrams indicating the observed locations of the wave fronts and associated active regions, and the speeds of the wave fronts. The measured speeds of the wave fronts varied from less than 50 to over 700 km s -1 with 'typical' speeds of 200-400 km s -1 .

  16. Evidence linking coronal mass ejections with interplanetary magnetic clouds

    International Nuclear Information System (INIS)

    Wilson, R.M.; Hildner, E.

    1983-12-01

    Using proxy data for the occurrence of those mass ejections from the solar corona which are directed earthward, we investigate the association between the post-1970 interplanetary magnetic clouds of Klein and Burlaga and coronal mass ejections. The evidence linking magnetic clouds following shocks with coronal mass ejections is striking. Six of nine clouds observed at Earth were preceded an appropriate time earlier by meter-wave type II radio bursts indicative of coronal shock waves and coronal mass ejections occurring near central meridian. During the selected periods when no clouds were detected near Earth, the only type II bursts reported were associated with solar activity near the limbs. Where the proxy solar data to be sought are not so clearly suggested, that is, for clouds preceding interaction regions and clouds within cold magnetic enhancements, the evidence linking the clouds and coronal mass ejections is not as clear proxy data usually suggest many candidate mass-ejection events for each cloud. Overall, the data are consistent with and support the hypothesis suggested by Klein and Burlaga that magnetic clouds observed with spacecraft at 1 AU are manifestations of solar coronal mass ejection transients

  17. New Evidence that Magnetoconvection Drives Solar–Stellar Coronal Heating

    Energy Technology Data Exchange (ETDEWEB)

    Tiwari, Sanjiv K.; Panesar, Navdeep K.; Moore, Ronald L.; Winebarger, Amy R. [NASA Marshall Space Flight Center, Mail Code ST 13, Huntsville, AL 35812 (United States); Thalmann, Julia K., E-mail: sanjivtiwari80@gmail.com [Institute of Physics/IGAM, University of Graz, Universittsplatz 5/II, A-8010 Graz (Austria)

    2017-07-10

    How magnetic energy is injected and released in the solar corona, keeping it heated to several million degrees, remains elusive. Coronal heating generally increases with increasing magnetic field strength. From a comparison of a nonlinear force-free model of the three-dimensional active region coronal field to observed extreme-ultraviolet loops, we find that (1) umbra-to-umbra coronal loops, despite being rooted in the strongest magnetic flux, are invisible, and (2) the brightest loops have one foot in an umbra or penumbra and the other foot in another sunspot’s penumbra or in unipolar or mixed-polarity plage. The invisibility of umbra-to-umbra loops is new evidence that magnetoconvection drives solar-stellar coronal heating: evidently, the strong umbral field at both ends quenches the magnetoconvection and hence the heating. Broadly, our results indicate that depending on the field strength in both feet, the photospheric feet of a coronal loop on any convective star can either engender or quench coronal heating in the loop’s body.

  18. THE CORONAL ABUNDANCES OF MID-F DWARFS

    International Nuclear Information System (INIS)

    Wood, Brian E.; Laming, J. Martin

    2013-01-01

    A Chandra spectrum of the moderately active nearby F6 V star π 3 Ori is used to study the coronal properties of mid-F dwarfs. We find that π 3 Ori's coronal emission measure distribution is very similar to those of moderately active G and K dwarfs, with an emission measure peak near log T = 6.6 seeming to be ubiquitous for such stars. In contrast to coronal temperature, coronal abundances are known to depend on spectral type for main sequence stars. Based on this previously known relation, we expected π 3 Ori's corona to exhibit an extremely strong ''first ionization potential (FIP) effect'', a phenomenon first identified on the Sun where elements with low FIP are enhanced in the corona. We instead find that π 3 Ori's corona exhibits a FIP effect essentially identical to that of the Sun and other early G dwarfs, perhaps indicating that the increase in FIP bias toward earlier spectral types stops or at least slows for F stars. We find that π 3 Ori's coronal characteristics are significantly different from two previously studied mid-F stars, Procyon (F5 IV-V) and τ Boo (F7 V). We believe π 3 Ori is more representative of the coronal characteristics of mid-F dwarfs, with Procyon being different because of luminosity class, and τ Boo being different because of the effects of one of two close companions, one stellar (τ Boo B: M2 V) and one planetary.

  19. Estrabismo em idade ambliogénica: estudo retrospectivo de 12 meses consecutivos de referenciação oftalmológica hospitalar

    OpenAIRE

    Monteiro, Sílvia

    2017-01-01

    Introdução: O objectivo deste trabalho é a análise do estado actual da referenciação oftalmológica hospitalar de casos de estrabismo em idade pediátrica.Métodos: Estudo retrospectivo e descritivo dos processos clínicos das crianças com idade menor ou igual a 10 anos referenciadas à Consulta de Oftalmologia Pediátrica do Centro Hospitalar do Porto entre Julho de 2011 e Julho de 2012.Resultados: Das 649 crianças referenciadas, 267 (41.1%) foram por suspeita de estrabismo. Em 109 (40.8%) dessas ...

  20. ON THE RELATIONSHIP BETWEEN THE CORONAL MAGNETIC DECAY INDEX AND CORONAL MASS EJECTION SPEED

    Energy Technology Data Exchange (ETDEWEB)

    Xu Yan; Liu Chang; Jing Ju; Wang Haimin, E-mail: yx2@njit.edu [Space Weather Research Lab, Center for Solar-Terrestrial Research, New Jersey Institute of Technology, 323 Martin Luther King Boulevard, Newark, NJ 07102-1982 (United States)

    2012-12-10

    Numerical simulations suggest that kink and torus instabilities are two potential contributors to the initiation and prorogation of eruptive events. A magnetic parameter called the decay index (i.e., the coronal magnetic gradient of the overlying fields above the eruptive flux ropes) could play an important role in controlling the kinematics of eruptions. Previous studies have identified a threshold range of the decay index that distinguishes between eruptive and confined configurations. Here we advance the study by investigating if there is a clear correlation between the decay index and coronal mass ejection (CME) speed. Thirty-eight CMEs associated with filament eruptions and/or two-ribbon flares are selected using the H{alpha} data from the Global H{alpha} Network. The filaments and flare ribbons observed in H{alpha} associated with the CMEs help to locate the magnetic polarity inversion line, along which the decay index is calculated based on the potential field extrapolation using Michelson Doppler Imager magnetograms as boundary conditions. The speeds of CMEs are obtained from the LASCO C2 CME catalog available online. We find that the mean decay index increases with CME speed for those CMEs with a speed below 1000 km s{sup -1} and stays flat around 2.2 for the CMEs with higher speeds. In addition, we present a case study of a partial filament eruption, in which the decay indices show different values above the erupted/non-erupted part.

  1. The Longitudinal Evolution of Equatorial Coronal Holes

    Science.gov (United States)

    Krista, Larisza D.; McIntosh, Scott W.; Leamon, Robert J.

    2018-04-01

    In 2011, three satellites—the Solar-Terrestrial RElations Observatory A & B, and the Solar Dynamics Observatory (SDO)—were in a unique spatial alignment that allowed a 360° view of the Sun. This alignment lasted until 2014, the peak of solar cycle 24. Using extreme ultraviolet images and Hovmöller diagrams, we studied the lifetimes and propagation characteristics of coronal holes (CHs) in longitude over several solar rotations. Our initial results show at least three distinct populations of “low-latitude” or “equatorial” CHs (below 65^\\circ latitude). One population rotates in retrograde direction and coincides with a group of long-lived (over sixty days) CHs in each hemisphere. These are typically located between 30° and 55^\\circ , and display velocities of ∼55 m s‑1 slower than the local differential rotation rate. A second, smaller population of CHs rotate prograde, with velocities between ∼20 and 45 m s‑1. This population is also long-lived, but observed ±10° from the solar equator. A third population of CHs are short-lived (less than two solar rotations), and they appear over a wide range of latitudes (±65°) and exhibit velocities between ‑140 and 80 m s‑1. The CH “butterfly diagram” we developed shows a systematic evolution of the longer-lived holes; however, the sample is too short in time to draw conclusions about possible connections to dynamo-related phenomena. An extension of the present work to the 22 years of the combined SOHO–SDO archives is necessary to understand the contribution of CHs to the decadal-scale evolution of the Sun.

  2. Coronal mass ejections and solar radio bursts

    International Nuclear Information System (INIS)

    Kundu, M.R.

    1990-01-01

    The properties of coronal mass ejection (CME) events and their radio signatures are discussed. These signatures are mostly in the form of type II and type IV burst emissions. Although type II bursts are temporally associated with CMEs, it is shown that there is no spatial relationship between them. Type II's associated with CMEs have in most cases a different origin, and they are not piston-driven by CMEs. Moving type IV and type II bursts can be associated with slow CMEs with speeds as low as 200 km/s, contrary to the earlier belief that only CMEs with speeds >400 km/s are associated with radio bursts. A specific event has been discussed in which the CME and type IV burst has nearly the same speed and direction, but the type II burst location was behind the CME and its motion was transverse. The speed and motion of the type II burst strongly suggest that the type II shock was decoupled from the CME and was probably due to a flare behind the limb. Therefore only the type IV source could be directly associated with the slow CME. The electrons responsble for the type IV emission could be produced in the flare or in the type II and then become trapped in a plasmoid associated with the CME. The reconnected loop could then move outwards as in the usual palsmoid model. Alternatively, the type IV emission could be interpreted as due to electrons produced by acceleration in wave turbulence driven by currents in the shock front driven by the CME. The lower-hybrid model Lampe and Papadopoulos (1982), which operates at both fast and slow mode shocks, could be applied to this situation. (author). 31 refs., 12 figs

  3. CME Interaction with Coronal Holes and Their Interplanetary Consequences

    Science.gov (United States)

    Gopalswamy, N.; Makela, P.; Xie, H.; Akiyama, S.; Yashiro, S.

    2008-01-01

    A significant number of interplanetary (IP) shocks (-17%) during cycle 23 were not followed by drivers. The number of such "driverless" shocks steadily increased with the solar cycle with 15%, 33%, and 52% occurring in the rise, maximum, and declining phase of the solar cycle. The solar sources of 15% of the driverless shocks were very close the central meridian of the Sun (within approx.15deg), which is quite unexpected. More interestingly, all the driverless shocks with their solar sources near the solar disk center occurred during the declining phase of solar cycle 23. When we investigated the coronal environment of the source regions of driverless shocks, we found that in each case there was at least one coronal hole nearby suggesting that the coronal holes might have deflected the associated coronal mass ejections (CMEs) away from the Sun-Earth line. The presence of abundant low-latitude coronal holes during the declining phase further explains why CMEs originating close to the disk center mimic the limb CMEs, which normally lead to driverless shocks due to purely geometrical reasons. We also examined the solar source regions of shocks with drivers. For these, the coronal holes were located such that they either had no influence on the CME trajectories. or they deflected the CMEs towards the Sun-Earth line. We also obtained the open magnetic field distribution on the Sun by performing a potential field source surface extrapolation to the corona. It was found that the CMEs generally move away from the open magnetic field regions. The CME-coronal hole interaction must be widespread in the declining phase, and may have a significant impact on the geoeffectiveness of CMEs.

  4. Space- and Ground-based Coronal Spectro-Polarimetry

    Science.gov (United States)

    Fineschi, Silvano; Bemporad, Alessandro; Rybak, Jan; Capobianco, Gerardo

    This presentation gives an overview of the near-future perspectives of ultraviolet and visible-light spectro-polarimetric instrumentation for probing coronal magnetism from space-based and ground-based observatories. Spectro-polarimetric imaging of coronal emission-lines in the visible-light wavelength-band provides an important diagnostics tool of the coronal magnetism. The interpretation in terms of Hanle and Zeeman effect of the line-polarization in forbidden emission-lines yields information on the direction and strength of the coronal magnetic field. As study case, this presentation will describe the Torino Coronal Magnetograph (CorMag) for the spectro-polarimetric observation of the FeXIV, 530.3 nm, forbidden emission-line. CorMag - consisting of a Liquid Crystal (LC) Lyot filter and a LC linear polarimeter - has been recently installed on the Lomnicky Peak Observatory 20cm Zeiss coronagraph. The preliminary results from CorMag will be presented. The linear polarization by resonance scattering of coronal permitted line-emission in the ultraviolet (UV)can be modified by magnetic fields through the Hanle effect. Space-based UV spectro-polarimeters would provide an additional tool for the disgnostics of coronal magnetism. As a case study of space-borne UV spectro-polarimeters, this presentation will describe the future upgrade of the Sounding-rocket Coronagraphic Experiment (SCORE) to include the capability of imaging polarimetry of the HI Lyman-alpha, 121.6 nm. SCORE is a multi-wavelength imager for the emission-lines, HeII 30.4 nm and HI 121.6 nm, and visible-light broad-band emission of the polarized K-corona. SCORE has flown successfully in 2009. This presentation will describe how in future re-flights SCORE could observe the expected Hanle effect in corona with a HI Lyman-alpha polarimeter.

  5. Toxoplasmose em primatas neotropicais: estudo retrospectivo de sete casos Toxoplasmosis in New World primates: Retrospective study of seven cases

    Directory of Open Access Journals (Sweden)

    Renata A. Casagrande

    2013-01-01

    Full Text Available A toxoplasmose é considerada uma doença parasitária fatal em primatas neotropicais. O objetivo deste trabalho foi descrever, através de um estudo retrospectivo, os casos de toxoplasmose em primatas neotropicais. No período de 1999-2009 foram realizados 86 exames anatomopatológicos em primatas e a toxoplasmose foi a enfermidade mais comum (7/86, relatando-se um caso em sagui-do-tufo-preto (Callithrix penicillata e seis em bugio-ruivo (Alouatta guariba. Dois animais foram encontrados mortos e cinco morreram em poucos dias. Os sinais clínicos mais frequentes foram apatia e anorexia (5/7, distensão abdominal (4/7 e febre (3/7. Na necropsia observou-se esplenomegalia (4/7, hemorragia do trato digestório, linfonodos e bexiga (4/7, pulmões avermelhados (3/7 e hepatomegalia (2/7. No exame histopatológico evidenciou-se hepatite (7/7, esplenite (3/7, miocardite (2/7, enterite (2/7, linfadenite (1/7 e sialite (1/7 necróticas e, pneumonia intersticial (4/7. Em fígado, pulmões, baço, coração, linfonodos e glândula salivar havia taquizoítos de Toxoplasma gondii que foram também detectados pelo exame de imuno-histoquímica anti-T. gondii em fígado, baço e pulmões (5/7. A toxoplasmose pode causar alta mortalidade em colônias de primatas neotropicais e representar mais uma ameaça à conversação dessas espécies em cativeiro. Sendo assim, medidas preventivas devem ser tomadas para evitar a contaminação desses animais.Toxoplasmosis is considered to be a fatal parasitic disease in New World primates. The objective of this report was to describe, through a retrospective study, the toxoplasmosis cases in New World primates. From 1999 to 2009 eighty-six anatomopathological exams was performed in primates and toxoplasmosis was the most common disease (7/86. One case occurred in Black-Tufted-Marmoset (Callithrix penicillata and six in Brown-Howler monkeys (Alouatta guariba. Two monkeys were found death and five died within few days. The most

  6. Endometriose de cicatriz cirúrgica: estudo retrospectivo de 72 casos Scar endometriosis: a retrospective study of 72 patients

    Directory of Open Access Journals (Sweden)

    Nilo Sérgio Nominato

    2007-08-01

    Full Text Available OBJETIVO: avaliar a freqüência e fatores associados à endometriose de cicatriz cirúrgica. MÉTODOS: foi realizado estudo observacional, tipo coorte retrospectivo, a partir da revisão de prontuários de pacientes do Hospital das Clínicas da Universidade Federal de Minas Gerais (UFMG com diagnóstico anatomopatológico de endometriose de cicatriz cirúrgica, no período de maio de 1978 a dezembro de 2003. RESULTADOS: foram encontrados 72 pacientes com diagnóstico de endometriose de cicatriz. A incidência de endometriose de cicatriz após cesariana foi significativamente maior do que após parto normal (0,2 e 0,06%, respectivamente; pPURPOSE: to identify the incidence and associated factors of surgical scar endometriosis. METHODS: a retrospective cohort observational study performed from the medical records of female patients attended at the Clinical Hospital of Univesidade Federal de Minas Gerais (UFMG with histopathological diagnosis of scar endometriosis from May 1978 to December 2003. RESULTS: a total of 72 patients were included in the study. The incidence of scar endometriosis after cesarean section was significantly higher than after episiotomy (0.2% and 0.06%, respectively; p<0.00001 with relative risk of 3.3. The women’s age, when diagnosed, ranged from 16 to 48 years old, (mean=30.8 years old. The scar location varied according to the previous surgery: 46 scars after cesarean sections, one after hysterectomy and one after abdominal surgery (48 lesions in the abdominal wall; 19 scars after episiotomy, one because of relapse and two after pelvic floor surgeries (22 pelvic wounds; two women had not been submitted to previous gynecological surgery (one umbilical endometrioma and one lesion in the posterior vaginal wall. Pain was the most frequent symptom (80%, followed by a node (79% and, in more than 40%, the pain and the node suffered modification with menstruation. Other less frequent complaints were: dyspareunia, secondary

  7. MEXCODE* CASO DE ESTUDIO

    Directory of Open Access Journals (Sweden)

    Gabriel Arturo García Gómez

    2000-01-01

    Full Text Available El caso plantea la reactivación de un proyecto que se presentó en el año 1995 como alternativa para el desarrollo del centro del Valle y mejora de la eficiencia en el manejo del comercio exterior de la Cuenca Pacífica. El proyecto se revivió a raíz de la necesidad de la compañía patrocinadora de mejorar sus flujos de caja proyectados y la reciente autorización para su funcionamiento. El proyecto es el popularmente denominado “Puerto Seco” de la ciudad de Guadalajara de Buga, internamente nombrado Mexcode. Los estudios iniciales estaban encaminados a que el proyecto fuera manejado por el municipio de Buga, sin embargo, posteriormente se vio la necesidad de buscar que pasara a manos de la empresa privada. El municipio, después de analizar las propuestas de varios inversionistas de la región en las cuales se evaluaba la ubicación dentro de la zona de los predios de sus empresas, su área, proximidad a la línea férrea y a la doble calzada Buga-Tuluá (sitio de paso del 80% de la carga de importación y exportación por Buenaventura y evaluar aspectos relativos a su trayectoria empresarial y compromiso con el desarrollo de la región, decidió otorgarle el proyecto al Grupo Empresarial Agri-Supplies S.A.

  8. Estudio del CH interestelar

    Science.gov (United States)

    Olano, C.; Lemarchand, G.; Sanz, A. J.; Bava, J. A.

    El objetivo principal de este proyecto consiste en el estudio de la distribución y abundancia del CH en nubes interestelares a través de la observación de las líneas hiperfinas del CH en 3,3 GHz. El CH es una molécula de amplia distribución en el espacio interestelar y una de las pocas especies que han sido observadas tanto con técnicas de radio como ópticas. Desde el punto de vista tecnológico se ha desarrollado un cabezal de receptor que permitirá la realización de observaciones polarimétricas en la frecuencia de 3,3 GHz, con una temperatura del sistema de 60 K y un ancho de banda de 140 MHz, y que será instalado en el foco primario de la antena parabólica del IAR. El cabezal del receptor es capaz de detectar señales polarizadas, separando las componentes de polarización circular derecha e izquierda. Para tal fin el cabezal consta de dos ramas receptoras que amplificarán la señal y la trasladarán a una frecuencia más baja (frecuencia intermedia), permitiendo de esa forma un mejor transporte de la señal a la sala de control para su posterior procesamiento. El receptor además de tener características polarimétricas, podrá ser usado en el continuo y en la línea, utilizando las ventajas observacionales y de procesamiento de señal que actualmente posee el IAR.

  9. Optimizing Global Coronal Magnetic Field Models Using Image-Based Constraints

    Science.gov (United States)

    Jones-Mecholsky, Shaela I.; Davila, Joseph M.; Uritskiy, Vadim

    2016-01-01

    The coronal magnetic field directly or indirectly affects a majority of the phenomena studied in the heliosphere. It provides energy for coronal heating, controls the release of coronal mass ejections, and drives heliospheric and magnetospheric activity, yet the coronal magnetic field itself has proven difficult to measure. This difficulty has prompted a decades-long effort to develop accurate, timely, models of the field, an effort that continues today. We have developed a method for improving global coronal magnetic field models by incorporating the type of morphological constraints that could be derived from coronal images. Here we report promising initial tests of this approach on two theoretical problems, and discuss opportunities for application.

  10. Coronal Loop Evolution Observed with AIA and Hi-C

    Science.gov (United States)

    Mulu-Moore, Fana; Winebarger, A.; Cirtain, J.; Kobayashi, K.; Korreck, K.; Golub, L.; Kuzin. S.; Walsh, R.; DeForest, C.; DePontieu, B.; hide

    2012-01-01

    Despite much progress toward understanding the dynamics of the solar corona, the physical properties of coronal loops are not yet fully understood. Recent investigations and observations from different instruments have yielded contradictory results about the true physical properties of coronal loops. In the past, the evolution of loops has been used to infer the loop substructure. With the recent launch of High Resolution Coronal Imager (Hi-C), this inference can be validated. In this poster we discuss the first results of loop analysis comparing AIA and Hi-C data. We find signatures of cooling in a pixel selected along a loop structure in the AIA multi-filter observations. However, unlike previous studies, we find that the cooling time is much longer than the draining time. This is inconsistent with previous cooling models.

  11. Examining the Properties of Jets in Coronal Holes

    Science.gov (United States)

    Gaulle, Owen; Adams, Mitzi L.; Tennant, A. F.

    2012-01-01

    We examined both X-ray and Magnetic field data in order to determine if there is a correlation between emerging magnetic flux and the production of Coronal jets. It was proposed that emerging flux can be a trigger to a coronal jet. The jet is thought to be caused when local bipoles reconnect or when a region of magnetic polarity emerges through a uniform field. In total we studied 15 different jets that occurred over a two day period starting 2011-02-27 00:00:00 UTC and ending 2011-02-28 23:59:55 UTC. All of the jets were contained within a coronal hole that was centered on the disk. Of the 15 that we studied 6 were shown to have an increase of magnetic flux within one hour prior to the creation of the jet and 10 were within 3 hours before the event.

  12. Influence of coronal holes on CMEs in causing SEP events

    International Nuclear Information System (INIS)

    Shen Chenglong; Yao Jia; Wang Yuming; Ye Pinzhong; Wang Shui; Zhao Xuepu

    2010-01-01

    The issue of the influence of coronal holes (CHs) on coronal mass ejections (CMEs) in causing solar energetic particle (SEP) events is revisited. It is a continuation and extension of our previous work, in which no evident effects of CHs on CMEs in generating SEPs were found by statistically investigating 56 CME events. This result is consistent with the conclusion obtained by Kahler in 2004. We extrapolate the coronal magnetic field, define CHs as the regions consisting of only open magnetic field lines and perform a similar analysis on this issue for 76 events in total by extending the study interval to the end of 2008. Three key parameters, CH proximity, CH area and CH relative position, are involved in the analysis. The new result confirms the previous conclusion that CHs did not show any evident effect on CMEs in causing SEP events. (research papers)

  13. The origin of coronal lines in Seyfert galaxies

    International Nuclear Information System (INIS)

    Korista, K.T.; Ferland, G.J.

    1989-01-01

    This paper examines the possibility that the coronal line region in Seyfert galaxies may be the result of an interstellar medium (ISM) exposed to, and subsequently photoionized by, a 'bare' Seyfert nucleus. It is shown that a 'generic' AGN continuum illuminating the warm-phase of the ISM of a spiral galaxy can produce the observed emission. In this picture the same UV-radiation cone that is responsible for the high-excitation extended narrow-line emission clouds observed out to 1-2 kpc or farther from the nuclei of some Seyfert galaxies also produces the coronal lines. Soft X-rays originating in the nucleus are Compton-scattered off the ISM, thus producing extended soft X-ray emission, as observed in NGC 4151. The results of the calculations show a basic insensitivity to the ISM density, which explains why similar coronal line spectra are found in many Seyfert galaxies of varying physical environments. 60 refs

  14. CORONAL MASS EJECTION INDUCED OUTFLOWS OBSERVED WITH HINODE/EIS

    International Nuclear Information System (INIS)

    Jin, M.; Ding, M. D.; Chen, P. F.; Fang, C.; Imada, S.

    2009-01-01

    We investigate the outflows associated with two halo coronal mass ejections (CMEs) that occurred on 2006 December 13 and 14 in NOAA 10930, using the Hinode/EIS observations. Each CME was accompanied by an EIT wave and coronal dimmings. Dopplergrams in the dimming regions are obtained from the spectra of seven EIS lines. The results show that strong outflows are visible in the dimming regions during the CME eruption at different heights from the lower transition region to the corona. It is found that the velocity is positively correlated with the photospheric magnetic field, as well as the magnitude of the dimming. We estimate the mass loss based on height-dependent EUV dimmings and find it to be smaller than the CME mass derived from white-light observations. The mass difference is attributed partly to the uncertain atmospheric model, and partly to the transition region outflows, which refill the coronal dimmings.

  15. Coronal seismology waves and oscillations in stellar coronae

    CERN Document Server

    Stepanov, Alexander; Nakariakov, Valery M

    2012-01-01

    This concise and systematic account of the current state of this new branch of astrophysics presents the theoretical foundations of plasma astrophysics, magneto-hydrodynamics and coronal magnetic structures, taking into account the full range of available observation techniques -- from radio to gamma. The book discusses stellar loops during flare energy releases, MHD waves and oscillations, plasma instabilities and heating and charged particle acceleration. Current trends and developments in MHD seismology of solar and stellar coronal plasma systems are also covered, while recent p

  16. Thermal instabilities in magnetically confined plasmas: Solar coronal loops

    International Nuclear Information System (INIS)

    Habbal, S.R.; Rosner, R.

    1979-01-01

    The thermal stability of confined solar coronal structures (''loops'') is investigated, following both normal mode and a new, global instability analysis. We demonstrate that: (a) normal mode analysis shows modes with size scales comparable to that of loops to be unstable, but to be strongly affected by the loop boundary conditions; (b) a global analysis, based upon variation of the total loop energy losses and gains, yields loop stability conditions for global modes dependent upon the coronal loop heating process, with magnetically coupled heating processes giving marginal stability. The connection between the present analysis and the minimum flux corona of Hearn is also discussed

  17. Comparison of Two Coronal Magnetic Field Models to Reconstruct a Sigmoidal Solar Active Region with Coronal Loops

    Energy Technology Data Exchange (ETDEWEB)

    Duan, Aiying; Zhang, Huai [Key Laboratory of Computational Geodynamics, University of Chinese Academy of Sciences, Beijing 100049 (China); Jiang, Chaowei [Institute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, 518055 (China); Hu, Qiang; Gary, G. Allen; Wu, S. T. [Center for Space Plasma and Aeronomic Research, The University of Alabama in Huntsville, Huntsville, AL 35899 (United States); Cao, Jinbin, E-mail: duanaiying@ucas.ac.cn, E-mail: hzhang@ucas.ac.cn, E-mail: chaowei@hit.edu.cn [School of Space and Environment, Beihang University, Beijing 100191 (China)

    2017-06-20

    Magnetic field extrapolation is an important tool to study the three-dimensional (3D) solar coronal magnetic field, which is difficult to directly measure. Various analytic models and numerical codes exist, but their results often drastically differ. Thus, a critical comparison of the modeled magnetic field lines with the observed coronal loops is strongly required to establish the credibility of the model. Here we compare two different non-potential extrapolation codes, a nonlinear force-free field code (CESE–MHD–NLFFF) and a non-force-free field (NFFF) code, in modeling a solar active region (AR) that has a sigmoidal configuration just before a major flare erupted from the region. A 2D coronal-loop tracing and fitting method is employed to study the 3D misalignment angles between the extrapolated magnetic field lines and the EUV loops as imaged by SDO /AIA. It is found that the CESE–MHD–NLFFF code with preprocessed magnetogram performs the best, outputting a field that matches the coronal loops in the AR core imaged in AIA 94 Å with a misalignment angle of ∼10°. This suggests that the CESE–MHD–NLFFF code, even without using the information of the coronal loops in constraining the magnetic field, performs as good as some coronal-loop forward-fitting models. For the loops as imaged by AIA 171 Å in the outskirts of the AR, all the codes including the potential field give comparable results of the mean misalignment angle (∼30°). Thus, further improvement of the codes is needed for a better reconstruction of the long loops enveloping the core region.

  18. Estudios Experimentales 2 Parte: Estudios Cuasi-Experimentales

    OpenAIRE

    Manterola, Carlos; Otzen, Tamara

    2015-01-01

    Los estudios experimentales, se caracterizan por la valoración del efecto de una o más intervenciones, habitualmente de forma comparativa con otra intervención, o un placebo; y el carácter prospectivo, de la recolección de datos y seguimiento. Agrupados bajo esta denominación, existe una diversidad de diseños, entre los que se encuentran los estudios cuasi-experimentales (ECE), que se caracterizan especialmente por la ausencia de asignación aleatoria. El objetivo de este manuscrito, es report...

  19. More Macrospicule Jets in On-Disk Coronal Holes

    Science.gov (United States)

    Adams, M. L.; Sterling, A. C.; Moore, R. L.

    2015-01-01

    We examine the magnetic structure and dynamics of multiple jets found in coronal holes close to or on disk center. All data are from the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI) of the Solar Dynamics Observatory (SDO). We report on observations of about ten jets in an equatorial coronal hole spanning 2011 February 27 and 28. We show the evolution of these jets in AIA 193 A, examine the magnetic field configuration and flux changes in the jet area, and discuss the probable trigger mechanism of these events. We reported on another jet in this same coronal hole on 2011 February 27, (is) approximately 13:04 UT (Adams et al 2014, ApJ, 783: 11). That jet is a previously-unrecognized variety of blowout jet, in which the base-edge bright point is a miniature filament-eruption flare arcade made by internal reconnection of the legs of the erupting field. In contrast, in the presently-accepted 'standard' picture for blowout jets, the base-edge bright point is made by interchange reconnection of initially-closed erupting jet-base field with ambient open field. This poster presents further evidence of the production of the base-edge bright point in blowout jets by internal reconnection. Our observations suggest that most of the bigger and brighter EUV jets in coronal holes are blowout jets of the new-found variety.

  20. CLOSED-FIELD CORONAL HEATING DRIVEN BY WAVE TURBULENCE

    Energy Technology Data Exchange (ETDEWEB)

    Downs, Cooper; Lionello, Roberto; Mikić, Zoran; Linker, Jon A [Predictive Science Incorporated, 9990 Mesa Rim Rd. Suite 170, San Diego, CA 92121 (United States); Velli, Marco, E-mail: cdowns@predsci.com [EPSS, UCLA, Los Angeles, CA 90095 (United States)

    2016-12-01

    To simulate the energy balance of coronal plasmas on macroscopic scales, we often require the specification of the coronal heating mechanism in some functional form. To go beyond empirical formulations and to build a more physically motivated heating function, we investigate the wave-turbulence-driven (WTD) phenomenology for the heating of closed coronal loops. Our implementation is designed to capture the large-scale propagation, reflection, and dissipation of wave turbulence along a loop. The parameter space of this model is explored by solving the coupled WTD and hydrodynamic evolution in 1D for an idealized loop. The relevance to a range of solar conditions is also established by computing solutions for over one hundred loops extracted from a realistic 3D coronal field. Due to the implicit dependence of the WTD heating model on loop geometry and plasma properties along the loop and at the footpoints, we find that this model can significantly reduce the number of free parameters when compared to traditional empirical heating models, and still robustly describe a broad range of quiet-Sun and active region conditions. The importance of the self-reflection term in producing relatively short heating scale heights and thermal nonequilibrium cycles is also discussed.

  1. Magnetic Source Regions of Coronal Mass Ejections Brigitte ...

    Indian Academy of Sciences (India)

    2003) or two rows of opposite polarity field extending to ... sional Alfvén waves which bring up helicity from the sub-photospheric part of the flux tube ... Figure 1. Loss of equilibrium model: sketches of coronal field lines showing ... lines of the quadrupolar reconnection before the flare, (bottom left): TRACE observations of the.

  2. Automated coronal hole identification via multi-thermal intensity segmentation

    Science.gov (United States)

    Garton, Tadhg M.; Gallagher, Peter T.; Murray, Sophie A.

    2018-01-01

    Coronal holes (CH) are regions of open magnetic fields that appear as dark areas in the solar corona due to their low density and temperature compared to the surrounding quiet corona. To date, accurate identification and segmentation of CHs has been a difficult task due to their comparable intensity to local quiet Sun regions. Current segmentation methods typically rely on the use of single Extreme Ultra-Violet passband and magnetogram images to extract CH information. Here, the coronal hole identification via multi-thermal emission recognition algorithm (CHIMERA) is described, which analyses multi-thermal images from the atmospheric image assembly (AIA) onboard the solar dynamics observatory (SDO) to segment coronal hole boundaries by their intensity ratio across three passbands (171 Å, 193 Å, and 211 Å). The algorithm allows accurate extraction of CH boundaries and many of their properties, such as area, position, latitudinal and longitudinal width, and magnetic polarity of segmented CHs. From these properties, a clear linear relationship was identified between the duration of geomagnetic storms and coronal hole areas. CHIMERA can therefore form the basis of more accurate forecasting of the start and duration of geomagnetic storms.

  3. A Bayesian Approach to Period Searching in Solar Coronal Loops

    Energy Technology Data Exchange (ETDEWEB)

    Scherrer, Bryan; McKenzie, David [Montana State University, P.O. Box 173840 Bozeman, MT 59717-3840 (United States)

    2017-03-01

    We have applied a Bayesian generalized Lomb–Scargle period searching algorithm to movies of coronal loop images obtained with the Hinode X-ray Telescope (XRT) to search for evidence of periodicities that would indicate resonant heating of the loops. The algorithm makes as its only assumption that there is a single sinusoidal signal within each light curve of the data. Both the amplitudes and noise are taken as free parameters. It is argued that this procedure should be used alongside Fourier and wavelet analyses to more accurately extract periodic intensity modulations in coronal loops. The data analyzed are from XRT Observation Program 129C: “MHD Wave Heating (Thin Filters),” which occurred during 2006 November 13 and focused on active region 10293, which included coronal loops. The first data set spans approximately 10 min with an average cadence of 2 s, 2″ per pixel resolution, and used the Al-mesh analysis filter. The second data set spans approximately 4 min with a 3 s average cadence, 1″ per pixel resolution, and used the Al-poly analysis filter. The final data set spans approximately 22 min at a 6 s average cadence, and used the Al-poly analysis filter. In total, 55 periods of sinusoidal coronal loop oscillations between 5.5 and 59.6 s are discussed, supporting proposals in the literature that resonant absorption of magnetic waves is a viable mechanism for depositing energy in the corona.

  4. Microflares as Possible Sources for Coronal Heating Meera Gupta ...

    Indian Academy of Sciences (India)

    around 6.7 keV, which is an indicator of the presence of coronal plasma tem- perature ≥ 9 MK. On the other ... Key words. Solar flares: ... Details of SOXS mission, in-flight performance, calibration, instrumental response and background are ...

  5. Magnetic Field in the Gravitationally Stratified Coronal Loops B. N. ...

    Indian Academy of Sciences (India)

    field for the longest (L = 406 Mm) coronal loops. The magnetic fields Bstr and Babs also increase with the number density, if the loop length does not vary much. The increment in the magnetic field due to gravitational stratification is small at the lower number densities, however, it is large at the higher number densities.

  6. Initiation and Propagation of Coronal Mass Ejections P. F. Chen

    Indian Academy of Sciences (India)

    Introduction. Coronal mass ejections (CMEs) have been observed for over 30 years. They keep being an intriguing research topic, not only because they are now realized to be the major driver for space weather disturbances, which are intimately connected to human activities, but also because they themselves are full of ...

  7. Photometric Variability of Four Coronally Active Stars J. C. Pandey ...

    Indian Academy of Sciences (India)

    R. Narasimhan (Krishtel eMaging) 1461 1996 Oct 15 13:05:22

    ray surveys with the Einstein and the ROSAT observatories and found to be associated with bright late- type stars. Many of these stars have not been studied in detail for their chromospheric and coronal activity, and their nature is not fully ...

  8. RADIOLOGICAL TIPS Coronal views of the paediatric mandibular ...

    African Journals Online (AJOL)

    imaging. None of the cases subsequently revealed any evidence of traumatic brain injury on CTB but they all demonstrated mandibular condyle fractures best appreciated on coronal views. Axial (Fig. 1) ... T Peedikayil, MB ChB. Department of Radiology, Red Cross War Memorial Children's Hospital, Cape Town.

  9. Automated Identification of Coronal Holes from Synoptic EUV Maps

    Science.gov (United States)

    Hamada, Amr; Asikainen, Timo; Virtanen, Ilpo; Mursula, Kalevi

    2018-04-01

    Coronal holes (CHs) are regions of open magnetic field lines in the solar corona and the source of the fast solar wind. Understanding the evolution of coronal holes is critical for solar magnetism as well as for accurate space weather forecasts. We study the extreme ultraviolet (EUV) synoptic maps at three wavelengths (195 Å/193 Å, 171 Å and 304 Å) measured by the Solar and Heliospheric Observatory/Extreme Ultraviolet Imaging Telescope (SOHO/EIT) and the Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) instruments. The two datasets are first homogenized by scaling the SDO/AIA data to the SOHO/EIT level by means of histogram equalization. We then develop a novel automated method to identify CHs from these homogenized maps by determining the intensity threshold of CH regions separately for each synoptic map. This is done by identifying the best location and size of an image segment, which optimally contains portions of coronal holes and the surrounding quiet Sun allowing us to detect the momentary intensity threshold. Our method is thus able to adjust itself to the changing scale size of coronal holes and to temporally varying intensities. To make full use of the information in the three wavelengths we construct a composite CH distribution, which is more robust than distributions based on one wavelength. Using the composite CH dataset we discuss the temporal evolution of CHs during the Solar Cycles 23 and 24.

  10. Standing Slow MHD Waves in Radiatively Cooling Coronal Loops ...

    Indian Academy of Sciences (India)

    The standing slow magneto-acoustic oscillations in cooling coronal loops ... turbation and, eventually, reduces the MHD equations to a 1D system modelling ..... where the function Q is expanded in power series with respect to ǫ, i.e.,. Q = Q0 + ...

  11. OBSERVATIONAL SIGNATURES OF THE CORONAL KINK INSTABILITY WITH THERMAL CONDUCTION

    International Nuclear Information System (INIS)

    Botha, G. J. J.; Arber, T. D.; Srivastava, Abhishek K.

    2012-01-01

    It is known from numerical simulations that thermal conduction along magnetic field lines plays an important role in the evolution of the kink instability in coronal loops. This study presents the observational signatures of the kink instability in long coronal loops when parallel thermal conduction is included. The three-dimensional nonlinear magnetohydrodynamic equations are solved numerically to simulate the evolution of a coronal loop that is initially in an unstable equilibrium. The loop has length 80 Mm, width 8 Mm, and an initial maximum twist of Φ = 11.5π, where Φ is a function of the radius. The initial loop parameters are obtained from a highly twisted loop observed in the Transition Region and Coronal Explorer (TRACE) 171 Å wave band. Synthetic observables are generated from the data. These observables include spatial and temporal averaging to account for the resolution and exposure times of TRACE images. Parallel thermal conduction reduces the maximum local temperature by up to an order of magnitude. This means that different spectral lines are formed and different internal loop structures are visible with or without the inclusion of thermal conduction. However, the response functions sample a broad range of temperatures. The result is that the inclusion of parallel thermal conductivity does not have as large an impact on observational signatures as the order of magnitude reduction in the maximum temperature would suggest; the net effect is a blurring of internal features of the loop structure.

  12. Coronal Activity in the R CrA T Association

    Science.gov (United States)

    Patten, Brian M.; Oliversen, Ronald J. (Technical Monitor)

    2005-01-01

    Brian Patten is the Principal Investigator of the NASA ROSS-ADP project Coronal Activity in the R CrA T Association. For this project we have extracted net counts and variability information for all of the X-ray sources found in 23 archival ROSAT PSPC and HRI images in the region of the R CrA T association. These data have been merged with an extensive database of optical and near-infrared photometry, optical spectroscopy, and parallax data. These data have been used to (1) identify new association members and clarify the membership status of a number of previously suspected members of the association, and (2) derive, for the first time, an accurate coronal luminosity function for the T Tauri members of this T association and make direct comparisons between the coronal luminosity functions for other T associations and those of large clusters. We have used our survey data to assess (a) the importance of the star-formation environment in initial coronal activity levels, (b) the effects of PMS evolution on dynamo activity as a function of mass and age, and (c) the level of contamination by field post-T Tauri stars on association membership surveys.

  13. Analysis of Solar Coronal Holes with Synoptic Magnetogram Data

    Science.gov (United States)

    Canner, A.; Kim, T. K.; Pogorelov, N.; Yalim, M. S.

    2017-12-01

    Coronal holes are regions in which the magnetic field of the Sun is open with high magnetic flux and low plasma density. Because of the low plasma beta in these regions, the open field lines transport plasma from the Sun throughout the heliosphere. Coronal hole area is closely related to the expansion factor of the magnetic flux tube, as demonstrated by Tokumaru et al. (2017). Following the approach of Tokumaru et al. (2017), we employ a potential field source surface model to identify the open field regions on the photosphere and estimate the area and expansion factor for each coronal hole. While Tokumaru et al. (2017) analyzed synoptic maps from Kitt Peak National Observatory for the period 1995-2011, we use different magnetograph observations with higher spatial resolution (e.g., SOHO-MDI) for the same time period. We compare the coronal hole area - expansion factor relationship with the original results of Tokumaru et al (2017). This work was supported by the NSF-funded Research Experience for Undergraduates program "Solar and Heliospheric Physics at UAH and MSFC" run by the University of Alabama in Huntsville in partnership with the Marshall Space Flight Center through grant AGS-1460767.

  14. Merging of coronal and heliospheric numerical two dimensional MHD models

    Czech Academy of Sciences Publication Activity Database

    Odstrčil, Dušan; Linker, J. A.; Lionello, R.; Mikic, Z.; Riley, P.; Pizzo, J. V.; Luhmann, J. G.

    2002-01-01

    Roč. 107, A12 (2002), s. SSH14-1 - SSH14-11 ISSN 0148-0227 R&D Projects: GA AV ČR IAA3003003 Institutional research plan: CEZ:AV0Z1003909 Keywords : coronal mass ejection * interplanetary shock * numerical MHD simulation Subject RIV: BN - Astronomy, Celestial Mechanics, Astrophysics Impact factor: 2.245, year: 2002

  15. Solar wind heavy ions from energetic coronal events

    International Nuclear Information System (INIS)

    Bame, S.J.

    1978-01-01

    Ions heavier than those of He can be resolved in the solar wind with electrostatic E/q analyzers when the local thermal temperatures are low. Ordinarily this condition prevails in the low speed solar wind found between high speed streams, i.e. the interstream, IS, solar wind. Various ions of O, Si and Fe are resolved in IS heavy ion spectra. Relative ion peak intensities indicate that the O ionization state is established in the IS coronal source regions at approx. 2.1 x 10 6 K while the state of Fe is frozen in at approx. 1.5 x 10 6 K farther out. Occasionally, anomalous spectra are observed in which the usually third most prominent ion peak, O 8+ , is depressed as are the Fe peaks ranging from Fe 12+ to Fe 7+ . A prominent peak in the usual Si 8+ position of IS spectra is self-consistently shown to be Fe 16+ . These features demonstrate that the ionization states were frozen in at higher than usual coronal temperatures. The source regions of these hot heavy ion spectra are identified as energetic coronal events including flares and nonflare coronal mass ejections. 24 references

  16. Solar Magnetic Carpet III: Coronal Modelling of Synthetic Magnetograms

    Science.gov (United States)

    Meyer, K. A.; Mackay, D. H.; van Ballegooijen, A. A.; Parnell, C. E.

    2013-09-01

    This article is the third in a series working towards the construction of a realistic, evolving, non-linear force-free coronal-field model for the solar magnetic carpet. Here, we present preliminary results of 3D time-dependent simulations of the small-scale coronal field of the magnetic carpet. Four simulations are considered, each with the same evolving photospheric boundary condition: a 48-hour time series of synthetic magnetograms produced from the model of Meyer et al. ( Solar Phys. 272, 29, 2011). Three simulations include a uniform, overlying coronal magnetic field of differing strength, the fourth simulation includes no overlying field. The build-up, storage, and dissipation of magnetic energy within the simulations is studied. In particular, we study their dependence upon the evolution of the photospheric magnetic field and the strength of the overlying coronal field. We also consider where energy is stored and dissipated within the coronal field. The free magnetic energy built up is found to be more than sufficient to power small-scale, transient phenomena such as nanoflares and X-ray bright points, with the bulk of the free energy found to be stored low down, between 0.5 - 0.8 Mm. The energy dissipated is currently found to be too small to account for the heating of the entire quiet-Sun corona. However, the form and location of energy-dissipation regions qualitatively agree with what is observed on small scales on the Sun. Future MHD modelling using the same synthetic magnetograms may lead to a higher energy release.

  17. Coronal holes and high-speed wind streams

    International Nuclear Information System (INIS)

    Zirker, J.B.

    1977-01-01

    Coronal holes low have been identified as Bartel's M regions, i.e., sources of high-speed wind streams that produce recurrent geomagnetic variations. Throughout the Skylab period the polar caps of the Sun were coronal holes, and at lower latitudes the most persistent and recurrent holes were equatorial extensions of the polar caps. The holes rotated 'rigidly' at the equatorial synodic rate. They formed in regions of unipolar photospheric magnetic field, and their internal magnetic fields diverged rapidly with increasing distance from the sun. The geometry of the magnetic field in the inner corona seems to control both the physical properties of the holes and the global distribution of high-speed wind streams in the heliosphere. The latitude variation of the divergence of the coronal magnetic field lines produces corresponding variations in wind speed.During the years of declining solar activity the global field of the corona approximates a perturbed dipole. The divergence of field lines in each hemisphere produces a high-speed wind near the poles and low-speed wind in a narrow belt that coincides with the magnetic neutral sheet. The analysis of electron density measurements within a polar hole indicates that solar wind is accelerated principally in the region between 2 and 5 R/sub s/ and that mechanical wave pressure (possibly Alfven wave) may be responsible for the accleration of the wind. Phenomenological models for the birth and decay of coronal holes have been proposed. Attempts to explain the birth and rigid rotation of holes through dynamo action have been only partially successful. The 11-year variation of cosmic ray intensities at the earth may result from cyclic variation of open field regions associated with coronal holes

  18. FAST CONTRACTION OF CORONAL LOOPS AT THE FLARE PEAK

    International Nuclear Information System (INIS)

    Liu Rui; Wang Haimin

    2010-01-01

    On 2005 September 8, a coronal loop overlying the active region NOAA 10808 was observed in TRACE 171 A to contract at ∼100 km s -1 at the peak of an X5.4-2B flare at 21:05 UT. Prior to the fast contraction, the loop underwent a much slower contraction at ∼6 km s -1 for about 8 minutes, initiating during the flare preheating phase. The sudden switch to fast contraction is presumably corresponding to the onset of the impulsive phase. The contraction resulted in the oscillation of a group of loops located below, with the period of about 10 minutes. Meanwhile, the contracting loop exhibited a similar oscillatory pattern superimposed on the dominant downward motion. We suggest that the fast contraction reflects a suddenly reduced magnetic pressure underneath due either to (1) the eruption of magnetic structures located at lower altitudes or to (2) the rapid conversion of magnetic free energy in the flare core region. Electrons accelerated in the shrinking trap formed by the contracting loop can theoretically contribute to a late-phase hard X-ray burst, which is associated with Type IV radio emission. To complement the X5.4 flare which was probably confined, a similar event observed in SOHO/EIT 195 A on 2004 July 20 in an eruptive, M8.6 flare is briefly described, in which the contraction was followed by the expansion of the same loop leading up to a halo coronal mass ejection. These observations further substantiate the conjecture of coronal implosion and suggest coronal implosion as a new exciter mechanism for coronal loop oscillations.

  19. Features of solar wind streams on June 21-28, 2015 as a result of interactions between coronal mass ejections and recurrent streams from coronal holes

    Science.gov (United States)

    Shugay, Yu. S.; Slemzin, V. A.; Rod'kin, D. G.

    2017-11-01

    Coronal sources and parameters of solar wind streams during a strong and prolonged geomagnetic disturbance in June 2015 have been considered. Correspondence between coronal sources and solar wind streams at 1 AU has been determined using an analysis of solar images, catalogs of flares and coronal mass ejections, solar wind parameters including the ionic composition. The sources of disturbances in the considered period were a sequence of five coronal mass ejections that propagated along the recurrent solar wind streams from coronal holes. The observed differences from typical in magnetic and kinetic parameters of solar wind streams have been associated with the interactions of different types of solar wind. The ionic composition has proved to be a good additional marker for highlighting components in a mixture of solar wind streams, which can be associated with different coronal sources.

  20. Comorbilidad psicopatológica en el alcoholismo: un estudio descriptivo

    Directory of Open Access Journals (Sweden)

    Natalia Landa

    2006-01-01

    Full Text Available En este estudio se lleva a cabo un análisis del perfil de bebida y de la comorbilidad psicopatológica en 50 pacientes alcohólicos que acuden en busca de tratamiento a un programa ambulatorio de Proyecto Hombre de Navarra. Para ello, se lleva a cabo un estudio ex post facto, de carácter retrospectivo y con un grupo cuasi control. Se utilizan los criterios diagnósticos del DSM-IV-TR para la dependencia alcohólica, el Müncher Alkoholismus Test (MALT para valorar la gravedad del alcoholismo y el SCL-90-R como medida de la sintomatología asociada. Los resultados obtenidos muestran la presencia de numerosa sintomatología psicopatológica, con elevaciones significativas en la mayoría de las dimensiones del SCL-90-R, tanto en los hombres como en las mujeres de la muestra. La comparación con las muestras normativas refleja que los alcohólicos de la muestra presentan más síntomas psicopatológicos que la población normal, pero menos que la población psiquiátrica. Asimismo, la gravedad del alcoholismo se relaciona de forma significativa con la mayor presencia e intensidad de comorbilidad. Por último, se comentan las implicaciones de este estudio para la práctica clínica y para la investigación futura.

  1. The Relation between Coronal Holes and Coronal Mass Ejections during the Rise, Maximum, and Declining Phases of Solar Cycle 23

    Science.gov (United States)

    Mohamed, A. A.; Gopalswamy, N; Yashiro, S.; Akiyama, S.; Makela, P.; Xie, H.; Jung, H.

    2012-01-01

    We study the interaction between coronal holes (CHs) and coronal mass ejections (CMEs) using a resultant force exerted by all the coronal holes present on the disk and is defined as the coronal hole influence parameter (CHIP). The CHIP magnitude for each CH depends on the CH area, the distance between the CH centroid and the eruption region, and the average magnetic field within the CH at the photospheric level. The CHIP direction for each CH points from the CH centroid to the eruption region. We focus on Solar Cycle 23 CMEs originating from the disk center of the Sun (central meridian distance =15deg) and resulting in magnetic clouds (MCs) and non-MCs in the solar wind. The CHIP is found to be the smallest during the rise phase for MCs and non-MCs. The maximum phase has the largest CHIP value (2.9 G) for non-MCs. The CHIP is the largest (5.8 G) for driverless (DL) shocks, which are shocks at 1 AU with no discernible MC or non-MC. These results suggest that the behavior of non-MCs is similar to that of the DL shocks and different from that of MCs. In other words, the CHs may deflect the CMEs away from the Sun-Earth line and force them to behave like limb CMEs with DL shocks. This finding supports the idea that all CMEs may be flux ropes if viewed from an appropriate vantage point.

  2. PHYSICAL CONDITIONS OF CORONAL PLASMA AT THE TRANSIT OF A SHOCK DRIVEN BY A CORONAL MASS EJECTION

    Energy Technology Data Exchange (ETDEWEB)

    Susino, R.; Bemporad, A.; Mancuso, S., E-mail: susino@oato.inaf.it [INAF–Turin Astrophysical Observatory, via Osservatorio 20, I-10025 Pino Torinese (Italy)

    2015-10-20

    We report here on the determination of plasma physical parameters across a shock driven by a coronal mass ejection using white light (WL) coronagraphic images and radio dynamic spectra (RDS). The event analyzed here is the spectacular eruption that occurred on 2011 June 7, a fast CME followed by the ejection of columns of chromospheric plasma, part of them falling back to the solar surface, associated with a M2.5 flare and a type-II radio burst. Images acquired by the Solar and Heliospheric Observatory/LASCO coronagraphs (C2 and C3) were employed to track the CME-driven shock in the corona between 2–12 R{sub ⊙} in an angular interval of about 110°. In this interval we derived two-dimensional (2D) maps of electron density, shock velocity, and shock compression ratio, and we measured the shock inclination angle with respect to the radial direction. Under plausible assumptions, these quantities were used to infer 2D maps of shock Mach number M{sub A} and strength of coronal magnetic fields at the shock's heights. We found that in the early phases (2–4 R{sub ⊙}) the whole shock surface is super-Alfvénic, while later on (i.e., higher up) it becomes super-Alfvénic only at the nose. This is in agreement with the location for the source of the observed type-II burst, as inferred from RDS combined with the shock kinematic and coronal densities derived from WL. For the first time, a coronal shock is used to derive a 2D map of the coronal magnetic field strength over intervals of 10 R{sub ⊙} altitude and ∼110° latitude.

  3. Characteristics of Low-latitude Coronal Holes near the Maximum of Solar Cycle 24

    Energy Technology Data Exchange (ETDEWEB)

    Hofmeister, Stefan J.; Veronig, Astrid; Reiss, Martin A.; Temmer, Manuela [University of Graz, Institute of Physics, IGAM-Kanzelhöhe Observatory, Graz (Austria); Vennerstrom, Susanne [National Space Institute, DTU Space (Denmark); Vršnak, Bojan [Hvar Observatory, Faculty of Geodesy, Zagreb (Croatia); Heber, Bernd, E-mail: stefan.hofmeister@uni-graz.at [Universität Kiel, Institut für Experimentelle und Angewandte Physik, Kiel (Germany)

    2017-02-01

    We investigate the statistics of 288 low-latitude coronal holes extracted from SDO /AIA-193 filtergrams over the time range of 2011 January 01–2013 December 31. We analyze the distribution of characteristic coronal hole properties, such as the areas, mean AIA-193 intensities, and mean magnetic field densities, the local distribution of the SDO /AIA-193 intensity and the magnetic field within the coronal holes, and the distribution of magnetic flux tubes in coronal holes. We find that the mean magnetic field density of all coronal holes under study is 3.0 ± 1.6 G, and the percentaged unbalanced magnetic flux is 49 ± 16%. The mean magnetic field density, the mean unsigned magnetic field density, and the percentaged unbalanced magnetic flux of coronal holes depend strongly pairwise on each other, with correlation coefficients cc > 0.92. Furthermore, we find that the unbalanced magnetic flux of the coronal holes is predominantly concentrated in magnetic flux tubes: 38% (81%) of the unbalanced magnetic flux of coronal holes arises from only 1% (10%) of the coronal hole area, clustered in magnetic flux tubes with field strengths >50 G (10 G). The average magnetic field density and the unbalanced magnetic flux derived from the magnetic flux tubes correlate with the mean magnetic field density and the unbalanced magnetic flux of the overall coronal hole (cc>0.93). These findings give evidence that the overall magnetic characteristics of coronal holes are governed by the characteristics of the magnetic flux tubes.

  4. A model for radio emission from solar coronal shocks

    Energy Technology Data Exchange (ETDEWEB)

    Zhao, G. Q.; Chen, L.; Wu, D. J., E-mail: djwu@pmo.ac.cn [Purple Mountain Observatory, CAS, Nanjing 210008 (China)

    2014-05-01

    Solar coronal shocks are very common phenomena in the solar atmosphere and are believed to be the drivers of solar type II radio bursts. However, the microphysical nature of these emissions is still an open question. This paper proposes that electron cyclotron maser (ECM) emission is responsible for the generation of radiation from the coronal shocks. In the present model, an energetic ion beam accelerated by the shock first excites the Alfvén wave (AW), then the excited AW leads to the formation of a density-depleted duct along the foreshock boundary of the shock. In this density-depleted duct, the energetic electron beam produced via the shock acceleration can effectively excite radio emission by ECM instability. Our results show that this model may potentially be applied to solar type II radio bursts.

  5. A model for radio emission from solar coronal shocks

    International Nuclear Information System (INIS)

    Zhao, G. Q.; Chen, L.; Wu, D. J.

    2014-01-01

    Solar coronal shocks are very common phenomena in the solar atmosphere and are believed to be the drivers of solar type II radio bursts. However, the microphysical nature of these emissions is still an open question. This paper proposes that electron cyclotron maser (ECM) emission is responsible for the generation of radiation from the coronal shocks. In the present model, an energetic ion beam accelerated by the shock first excites the Alfvén wave (AW), then the excited AW leads to the formation of a density-depleted duct along the foreshock boundary of the shock. In this density-depleted duct, the energetic electron beam produced via the shock acceleration can effectively excite radio emission by ECM instability. Our results show that this model may potentially be applied to solar type II radio bursts.

  6. Radio and white-light observations of coronal transients

    Science.gov (United States)

    Dulk, G. A.

    1980-01-01

    Optical, radio and X-ray evidence of violent mass motions in the corona has existed for some years but only recently have the form, nature, frequency and implication of the transients become obvious. In this paper the observed properties of coronal transients are reviewed, with concentration on the white-light and radio manifestations. The classification according to speeds seems to be meaningful, with the slow transients having thermal emissions at radio wavelengths and the fast ones nonthermal. The possible mechanisms involved in the radio bursts are then discussed and estimates of various forms of energy are reviewed. It appears that the magnetic energy transported from the sun by the transient exceeds that of any other form, and that magnetic forces dominate in the dynamics of the motions. The conversion of magnetic energy into mechanical energy, by expansion of the field, provides a possible driving force for the coronal and interplanetary shock waves.

  7. Radio and white-light observations of coronal transients

    International Nuclear Information System (INIS)

    Dulk, G.A.

    1980-01-01

    Optical, radio and X-ray evidence of violent mass motions in the corona has existed for some years but only recently have the form, nature, frequency and implication of the transients become obvious. The author reviews the observed properties of coronal transients, concentrating on the white-light and radio manifestations. The classification according to speeds seems to be meaningful, with the slow transients having thermal emissions at radio wavelengths and the fast ones non-thermal. The possible mechanisms involved in the radio bursts are discussed and the estimates of various forms of energy are reviewed. It appears that the magnetic energy transported from the Sun by the transient exceeds that of any other form, and that magnetic forces dominate in the dynamics of the motions. The conversion of magnetic energy into mechanical energy, by expansion of the fields, provides a possible driving force for the coronal and interplanetary shock waves. (Auth.)

  8. Shear-induced inflation of coronal magnetic fields

    International Nuclear Information System (INIS)

    Klimchuk, J.A.

    1990-01-01

    Using numerical models of force-free magnetic fields, the shearing of footprints in arcade geometries leading to an inflation of the coronal magnetic field was examined. For each of the shear profiles considered, all of the field lines become elevated compared with the potential field. This includes cases where the shear is concentrated well away from the arcade axis, such that B(sub z), the component of field parallel to the axis, increases outward to produce an inward B(sub z) squared/8 pi magnetic pressure gradient force. These results contrast with an earlier claim, shown to be incorrect, that field lines can sometimes become depressed as a result of shear. It is conjectured that an inflation of the entire field will always result from the shearing of simple arcade configurations. These results have implications for prominence formation, the interplanetary magnetic flux, and possibly also coronal holes. 38 refs

  9. Swift X-ray monitoring of stellar coronal variability

    Science.gov (United States)

    Miller, Brendan; Hagen, Cedric; Gallo, Elena; Wright, Jason T.

    2018-01-01

    We used California Planet Search Ca II H and K core emission measurements to identify and characterize chromospheric activity cycles in a sample of main-sequence FGK stars. About a dozen of these with existing ROSAT archival data were targeted with Swift to obtain a current epoch X-ray flux. We find that coronal variability by a factor of several is common on decade-long timescales (we attempt to link to the chromospheric cycle phase) but can also occur on short timescales between Swift visits to a given target, presumably related to stellar rotation and coronal inhomogeneity or to small flares. Additionally, we present new Swift monitoring observations of two M dwarfs with known exoplanets: GJ 15A and GJ 674. GJ 15A b is around 5.3 Earth masses with an 11.4 day orbital period, while GJ 674 is around 11.1 Earth masses with a 4.7 day orbital period. GJ 15A was observed several times in late 2014 and then monitored at approximately weekly intervals for several months in early 2016, for a total exposure of 18 ks. GJ 674 was monitored at approximately weekly intervals for most of 2016, for a total exposure of 40 ks. We provide light curves and hardness ratios for both sources, and also compare to earlier archival X-ray data. Both sources show significant X-ray variability, including between consecutive observations. We quantify the energy distribution for coronal flaring, and compare to optical results for M dwarfs from Kepler. Finally, we discuss the implications of M dwarf coronal activity for exoplanets orbiting within the nominal habitable zone.

  10. Morphology and physical properties of solar coronal holes

    International Nuclear Information System (INIS)

    Rozelot, J.P.

    1983-01-01

    By their peculiar characteristics, coronal holes induce on Earth climatic variations and cyclic effects, not well known nowadays. Because of low electronical density and very low temperature, study of these holes was neglected. The author presents the results of the observations from discovery in the fifteens. He gives some new results, a theoretical model and not well resolved questions which can conduct to new methods of searching [fr

  11. The evolution of coronal activity in main sequence cool stars

    International Nuclear Information System (INIS)

    Stern, R.A.

    1984-01-01

    Stars spend most of their lifetime and show the least amount of nuclear evolution on the main sequence. However, the x-ray luminosities of cool star coronas change by orders of magnitude as a function of main sequence age. Such coronal evolution is discussed in relation to our knowledge of the solar corona, solar and stellar flares, stellar rotation and binarity. The relevance of X-ray observations to current speculations on stellar dynamos is also considered

  12. PROJECTION EFFECTS IN CORONAL DIMMINGS AND ASSOCIATED EUV WAVE EVENT

    Energy Technology Data Exchange (ETDEWEB)

    Dissauer, K.; Temmer, M.; Veronig, A. M.; Vanninathan, K. [IGAM/Institute of Physics, University of Graz, Universitätsplatz 5/II, A-8010 Graz (Austria); Magdalenić, J., E-mail: karin.dissauer@uni-graz.at [Solar-Terrestrial Center of Excellence-SIDC, Royal Observatory of Belgium, Av. Circulaire 3, B-1180 Brussels (Belgium)

    2016-10-20

    We investigate the high-speed ( v > 1000 km s{sup −1}) extreme-ultraviolet (EUV) wave associated with an X1.2 flare and coronal mass ejection (CME) from NOAA active region 11283 on 2011 September 6 (SOL2011-09-06T22:12). This EUV wave features peculiar on-disk signatures; in particular, we observe an intermittent “disappearance” of the front for 120 s in Solar Dynamics Observatory ( SDO )/AIA 171, 193, 211 Å data, whereas the 335 Å filter, sensitive to hotter plasmas ( T ∼ 2.5 MK), shows a continuous evolution of the wave front. The eruption was also accompanied by localized coronal dimming regions. We exploit the multi-point quadrature position of SDO and STEREO-A , to make a thorough analysis of the EUV wave evolution, with respect to its kinematics and amplitude evolution and reconstruct the SDO line-of-sight (LOS) direction of the identified coronal dimming regions in STEREO-A . We show that the observed intensities of the dimming regions in SDO /AIA depend on the structures that are lying along their LOS and are the combination of their individual intensities, e.g., the expanding CME body, the enhanced EUV wave, and the CME front. In this context, we conclude that the intermittent disappearance of the EUV wave in the AIA 171, 193, and 211 Å filters, which are channels sensitive to plasma with temperatures below ∼2 MK is also caused by such LOS integration effects. These observations clearly demonstrate that single-view image data provide us with limited insight to correctly interpret coronal features.

  13. Unambiguous Evidence of Coronal Implosions during Solar Eruptions and Flares

    Science.gov (United States)

    Wang, Juntao; Simões, P. J. A.; Fletcher, L.

    2018-05-01

    In the implosion conjecture, coronal loops contract as the result of magnetic energy release in solar eruptions and flares. However, after almost two decades, observations of this phenomenon are still rare and most previous reports are plagued by projection effects so that loop contraction could be either true implosion or just a change in loop inclination. In this paper, to demonstrate the reality of loop contractions in the global coronal dynamics, we present four events with the continuously contracting loops in an almost edge-on geometry from the perspective of SDO/AIA, which are free from the ambiguity caused by the projection effects, also supplemented by contemporary observations from STEREO for examination. In the wider context of observations, simulations and theories, we argue that the implosion conjecture is valid in interpreting these events. Furthermore, distinct properties of the events allow us to identify two physical categories of implosion. One type demonstrates a rapid contraction at the beginning of the flare impulsive phase, as magnetic free energy is removed rapidly by a filament eruption. The other type, which has no visible eruption, shows a continuous loop shrinkage during the entire flare impulsive phase, which we suggest shows the ongoing conversion of magnetic free energy in a coronal volume. Corresponding scenarios are described that can provide reasonable explanations for the observations. We also point out that implosions may be suppressed in cases when a heavily mass-loaded filament is involved, possibly serving as an alternative account for their observational rarity.

  14. Macrospicule Jets in On-Disk Coronal Holes

    Science.gov (United States)

    Adams, M. L.; Sterling, A. C.; Moore, R. L.

    2014-01-01

    We examine the magnetic structure and dynamics of multiple jets found in coronal holes close to or on disk center. All data are from the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI) of the Solar Dynamics Observatory (SDO). We report on observations of six jets in an equatorial coronal hole spanning 2011 February 27 and 28. We show the evolution of these jets in AIA 193 A, examine the magnetic field configuration, and postulate the probable trigger mechanism of these events. We recently reported on another jet in the same coronal hole on 2011 February 27, approximately 13:04 Universal Time (Adams et al 2014, Astrophysical Journal, 783: 11); this jet is a previously-unrecognized variety of blowout jet. In this variety, the reconnection bright point is not made by interchange reconnection of initially-closed erupting field in the base of the jet with ambient open field. Instead, there is a miniature filament-eruption flare arcade made by internal reconnection of the legs of the erupting field.

  15. THE NATURE OF CME-FLARE-ASSOCIATED CORONAL DIMMING

    Energy Technology Data Exchange (ETDEWEB)

    Cheng, J. X. [Key Laboratory of Planetary Sciences, Shanghai Astronomical Observatory, Shanghai 200030 (China); Qiu, J., E-mail: chengjx@shao.ac.cn [Department of Physics, Montana State University, Bozeman MT 59717-3840 (United States)

    2016-07-01

    Coronal mass ejections (CMEs) are often accompanied by coronal dimming that is evident in extreme ultraviolet (EUV) and soft X-ray observations. The locations of dimming are sometimes considered to map footpoints of the erupting flux rope. As the emitting material expands in the corona, the decreased plasma density leads to reduced emission observed in spectral and irradiance measurements. Therefore, signatures of dimming may reflect the properties of CMEs in the early phase of their eruption. In this study, we analyze the event of flare, CME, and coronal dimming on 2011 December 26. We use the data from the Atmospheric Imaging Assembly on the Solar Dynamics Observatory for disk observations of the dimming, and analyze images taken by EUVI, COR1, and COR2 on board the Solar Terrestrial Relations Observatory to obtain the height and velocity of the associated CMEs observed at the limb. We also measure the magnetic reconnection rate from flare observations. Dimming occurs in a few locations next to the flare ribbons, and it is observed in multiple EUV passbands. Rapid dimming starts after the onset of fast reconnection and CME acceleration, and its evolution tracks the CME height and flare reconnection. The spatial distribution of dimming exhibits cores of deep dimming with a rapid growth, and their light curves are approximately linearly scaled with the CME height profile. From the dimming analysis we infer the process of the CME expansion, and estimate properties of the CME.

  16. Observable Signatures of Energy Release in Braided Coronal Loops

    Energy Technology Data Exchange (ETDEWEB)

    Pontin, D. I. [University of Dundee, Nethergate, Dundee, DD1 4HN (United Kingdom); Janvier, M. [Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Sud, Université Paris-Saclay, Bât. 121, F-91405, Orsay Cedex (France); Tiwari, S. K.; Winebarger, A. R.; Cirtain, J. W. [NASA Marshall Space Flight Center, ZP 13, Huntsville, AL 35812 (United States); Galsgaard, K. [Niels Bohr Institute, Geological Museum Østervoldgade 5-7, DK-1350, Copenhagen K (Denmark)

    2017-03-10

    We examine the turbulent relaxation of solar coronal loops containing non-trivial field line braiding. Such field line tangling in the corona has long been postulated in the context of coronal heating models. We focus on the observational signatures of energy release in such braided magnetic structures using MHD simulations and forward modeling tools. The aim is to answer the following question: if energy release occurs in a coronal loop containing braided magnetic flux, should we expect a clearly observable signature in emissions? We demonstrate that the presence of braided magnetic field lines does not guarantee a braided appearance to the observed intensities. Observed intensities may—but need not necessarily—reveal the underlying braided nature of the magnetic field, depending on the degree and pattern of the field line tangling within the loop. However, in all cases considered, the evolution of the braided loop is accompanied by localized heating regions as the loop relaxes. Factors that may influence the observational signatures are discussed. Recent high-resolution observations from Hi-C have claimed the first direct evidence of braided magnetic fields in the corona. Here we show that both the Hi-C data and some of our simulations give the appearance of braiding at a range of scales.

  17. Do coronal holes influence cosmic ray daily harmonics

    International Nuclear Information System (INIS)

    Ahluwalia, H.S.

    1977-01-01

    Coronal holes are identified by their low emissivity in either EUV (Munro and Withrobe, 1973) or in X-rays (Krieger et al, 1973). They are seats of unidirectional magnetic fields. Also, high speed solar wind streams originate in them. Also, high speed solar wind streams originate in then (Krieger et al, 1973; Neupert and Pizzo, 1974; Nolte et al, 1976). Coronal holes often extend over a wide range of heliolatitudes (Timothy et al, 1975). Elsewhere in the Proceedings we have presented results on the long term changes observed in the amplitudes and the times of maximum of the diurnal, the semidiurnal and the tridiurnal variations of cosmic rays, at low (neutrons) and at high (underground muons) primary rigidities (Ahluwalia, 1977). We have shown that a dramatic shift to early hours is noticeable in the times of maxima of the harmonics during 1971-72 period. In this paper we examine the nature of the contributions of off-ecliptic cosmic rays of high enough rigidity, streaming under the influence of large scale ordered interplanetary magnetic field set up by the coronal holes, to the cosmic ray daily harmonics. Some models are presented and discussed in a preliminary fashion. (author)

  18. MHD modeling of coronal loops: the transition region throat

    Science.gov (United States)

    Guarrasi, M.; Reale, F.; Orlando, S.; Mignone, A.; Klimchuk, J. A.

    2014-04-01

    Context. The expansion of coronal loops in the transition region may considerably influence the diagnostics of the plasma emission measure. The cross-sectional area of the loops is expected to depend on the temperature and pressure, and might be sensitive to the heating rate. Aims: The approach here is to study the area response to slow changes in the coronal heating rate, and check the current interpretation in terms of steady heating models. Methods: We study the area response with a time-dependent 2D magnetohydrodynamic (MHD) loop model, including the description of the expanding magnetic field, coronal heating and losses by thermal conduction, and radiation from optically thin plasma. We run a simulation for a loop 50 Mm long and quasi-statically heated to about 4 MK. Results: We find that the area can change substantially with the quasi-steady heating rate, e.g., by ~40% at 0.5 MK as the loop temperature varies between 1 MK and 4 MK, and, therefore, affects the interpretation of the differential emission measure vs. temperature (DEM(T)) curves. The movie associated to Fig. 4 is available in electronic form at http://www.aanda.org

  19. Comparison between two models of energy balance in coronal loops

    Science.gov (United States)

    Mac Cormack, C.; López Fuentes, M.; Vásquez, A. M.; Nuevo, F. A.; Frazin, R. A.; Landi, E.

    2017-10-01

    In this work we compare two models to analyze the energy balance along coronal magnetic loops. For the first stationary model we deduce an expression of the energy balance along the loops expressed in terms of quantities provided by the combination of differential emission measure tomography (DEMT) applied to EUV images time series and potential extrapolations of the coronal magnetic field. The second applied model is a 0D hydrodynamic model that provides the evolution of the average properties of the coronal plasma along the loops, using as input parameters the loop length and the heating rate obtained with the first model. We compare the models for two Carrington rotations (CR) corresponding to different periods of activity: CR 2081, corresponding to a period of minimum activity observed with the Extreme Ultraviolet Imager (EUVI) on board of the Solar Terrestrial Relations Observatory (STEREO), and CR 2099, corresponding to a period of activity increase observed with the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). The results of the models are consistent for both rotations.

  20. Numerically modelling the large scale coronal magnetic field

    Science.gov (United States)

    Panja, Mayukh; Nandi, Dibyendu

    2016-07-01

    The solar corona spews out vast amounts of magnetized plasma into the heliosphere which has a direct impact on the Earth's magnetosphere. Thus it is important that we develop an understanding of the dynamics of the solar corona. With our present technology it has not been possible to generate 3D magnetic maps of the solar corona; this warrants the use of numerical simulations to study the coronal magnetic field. A very popular method of doing this, is to extrapolate the photospheric magnetic field using NLFF or PFSS codes. However the extrapolations at different time intervals are completely independent of each other and do not capture the temporal evolution of magnetic fields. On the other hand full MHD simulations of the global coronal field, apart from being computationally very expensive would be physically less transparent, owing to the large number of free parameters that are typically used in such codes. This brings us to the Magneto-frictional model which is relatively simpler and computationally more economic. We have developed a Magnetofrictional Model, in 3D spherical polar co-ordinates to study the large scale global coronal field. Here we present studies of changing connectivities between active regions, in response to photospheric motions.

  1. Coronal Physics and the Chandra Emission Line Project

    Science.gov (United States)

    Brickhouse, N. S.; Drake, J. J.

    2000-01-01

    With the launch of the Chandra X-ray Observatory, high resolution X-ray spectroscopy of cosmic sources has begun. Early, deep observations of three stellar coronal sources Capella, Procyon, and HR 1099 are providing not only invaluable calibration data, but also benchmarks for plasma spectral models. These models are needed to interpret data from stellar coronae, galaxies and clusters of galaxies, supernova, remnants and other astrophysical sources. They have been called into question in recent years as problems with understanding low resolution ASCA and moderate resolution Extreme Ultraviolet Explorer Satellite (EUVE) data have arisen. The Emission Line Project is a collaborative effort, to improve the models, with Phase I being the comparison of models with observed spectra of Capella, Procyon, and HR 1099. Goals of these comparisons are (1) to determine and verify accurate and robust diagnostics and (2) to identify and prioritize issues in fundamental spectroscopy which will require further theoretical and/or laboratory work. A critical issue in exploiting the coronal data for these purposes is to understand the extent, to which common simplifying assumptions (coronal equilibrium, negligible optical depth) apply. We will discuss recent, advances in our understanding of stellar coronae, in this context.

  2. THE NATURE OF CME-FLARE-ASSOCIATED CORONAL DIMMING

    International Nuclear Information System (INIS)

    Cheng, J. X.; Qiu, J.

    2016-01-01

    Coronal mass ejections (CMEs) are often accompanied by coronal dimming that is evident in extreme ultraviolet (EUV) and soft X-ray observations. The locations of dimming are sometimes considered to map footpoints of the erupting flux rope. As the emitting material expands in the corona, the decreased plasma density leads to reduced emission observed in spectral and irradiance measurements. Therefore, signatures of dimming may reflect the properties of CMEs in the early phase of their eruption. In this study, we analyze the event of flare, CME, and coronal dimming on 2011 December 26. We use the data from the Atmospheric Imaging Assembly on the Solar Dynamics Observatory for disk observations of the dimming, and analyze images taken by EUVI, COR1, and COR2 on board the Solar Terrestrial Relations Observatory to obtain the height and velocity of the associated CMEs observed at the limb. We also measure the magnetic reconnection rate from flare observations. Dimming occurs in a few locations next to the flare ribbons, and it is observed in multiple EUV passbands. Rapid dimming starts after the onset of fast reconnection and CME acceleration, and its evolution tracks the CME height and flare reconnection. The spatial distribution of dimming exhibits cores of deep dimming with a rapid growth, and their light curves are approximately linearly scaled with the CME height profile. From the dimming analysis we infer the process of the CME expansion, and estimate properties of the CME.

  3. An Estimate of Solar Wind Velocity Profiles in a Coronal Hole and a Coronal Streamer Area (6-40 R(radius symbol)

    Science.gov (United States)

    Patzold, M.; Tsurutani, B. T.; Bird, M. K.

    1995-01-01

    Total electron content data obtained from the Ulysses Solar Corona Experiment (SCE) in 1991 were used to select two data sets, one associated with a coronal hole and the other with coronal streamer crossings. (This is largely equatorial data shortly after solar maximum.) The solar wind velocity profile is estimated for these areas.

  4. NO TRACE LEFT BEHIND: STEREO OBSERVATION OF A CORONAL MASS EJECTION WITHOUT LOW CORONAL SIGNATURES

    International Nuclear Information System (INIS)

    Robbrecht, Eva; Patsourakos, Spiros; Vourlidas, Angelos

    2009-01-01

    The availability of high-quality synoptic observations of the extreme-ultraviolet (EUV) and visible corona during the SOHO mission has advanced our understanding of the low corona manifestations of coronal mass ejections (CMEs). The EUV imager/white light coronagraph connection has been proven so powerful, it is routinely assumed that if no EUV signatures are present when a CME is observed by a coronagraph, then the event must originate behind the visible limb. This assumption carries strong implications for space weather forecasting but has not been put to the test. This paper presents the first detailed analysis of a frontside, large-scale CME that has no obvious counterparts in the low corona as observed in EUV and Hα wavelengths. The event was observed by the SECCHI instruments onboard the STEREO mission. The COR2A coronagraph observed a slow flux-rope-type CME, while an extremely faint partial halo was observed in COR2B. The event evolved very slowly and is typical of the streamer-blowout CME class. EUVI A 171 A images show a concave feature above the east limb, relatively stable for about two days before the eruption, when it rises into the coronagraphic fields and develops into the core of the CME. None of the typical low corona signatures of a CME (flaring, EUV dimming, filament eruption, waves) were observed in the EUVI B images, which we attribute to the unusually large height from which the flux rope lifted off. This interpretation is supported by the CME mass measurements and estimates of the expected EUV dimming intensity. Only thanks to the availability of the two viewpoints we were able to identify the likely source region. The event originated along a neutral line over the quiet-Sun. No active regions were present anywhere on the visible (from STEREO B) face of the disk. Leaving no trace behind on the solar disk, this observation shows unambiguously that a CME eruption does not need to have clear on-disk signatures. Also it sheds light on the

  5. Estudios sobre plantas andinas,- V

    Directory of Open Access Journals (Sweden)

    Cuatrecasas José

    1943-12-01

    Full Text Available Desde hace diez años, he venido interesándome por el conocimiento y clasificación del género Diplostephium, distribuido abundantemente en las zonas frías de los Andes, desde Venezuela al norte de Chile con un enclave en Costa Rica. Las excursiones realizadas en 1932 me permitieron descubrir dos nuevas especies colombianas (1 y el estudio de la colección Isern me dio oportunidad de conocer otras especies ecuatorianas y peruanas (2. A raíz del abundante material recogido en mis excursiones por Colombia desde el año 1938, decidí llevar a cabo el estudio monográfico del género; para ella diversos centros de los Estados Unidos pusieron a mi disposición sus coIecciones: Smithsonian Institution (United States National Herbarium, Field Museum of Natural History de Chicago y New York Botanical Garden, los cuales me remitieron el material para este fin al Instituto de Ciencias Naturales de Bogotá; el trabajo fue iniciado en este centro, pero al trasladarme a la Escuela Superior de Agricultura Tropical de Cali, la dirección del Instituto me permitió llevar para el Valle todos los ejemplares, incluso los del Herbario Nacional Colombiano, y así pude concluir el estudio provisional, en mi nuevo lugar de trabajo.

  6. FIELD TOPOLOGY ANALYSIS OF A LONG-LASTING CORONAL SIGMOID

    International Nuclear Information System (INIS)

    Savcheva, A. S.; Van Ballegooijen, A. A.; DeLuca, E. E.

    2012-01-01

    We present the first field topology analysis based on nonlinear force-free field (NLFFF) models of a long-lasting coronal sigmoid observed in 2007 February with the X-Ray Telescope on Hinode. The NLFFF models are built with the flux rope insertion method and give the three-dimensional coronal magnetic field as constrained by observed coronal loop structures and photospheric magnetograms. Based on these models, we have computed horizontal maps of the current and the squashing factor Q for 25 different heights in the corona for all six days of the evolution of the region. We use the squashing factor to quantify the degree of change of the field line linkage and to identify prominent quasi-separatrix layers (QSLs). We discuss the major properties of these QSL maps and devise a way to pick out important QSLs since our calculation cannot reach high values of Q. The complexity in the QSL maps reflects the high degree of fragmentation of the photospheric field. We find main QSLs and current concentrations that outline the flux rope cavity and that become characteristically S-shaped during the evolution of the sigmoid. We note that, although intermittent bald patches exist along the length of the sigmoid during its whole evolution, the flux rope remains stable for several days. However, shortly after the topology of the field exhibits hyperbolic flux tubes (HFT) on February 7 and February 12 the sigmoid loses equilibrium and produces two B-class flares and associated coronal mass ejections (CMEs). The location of the most elevated part of the HFT in our model coincides with the inferred locations of the two flares. Therefore, we suggest that the presence of an HFT in a coronal magnetic configuration may be an indication that the system is ready to erupt. We offer a scenario in which magnetic reconnection at the HFT drives the system toward the marginally stable state. Once this state is reached, loss of equilibrium occurs via the torus instability, producing a CME.

  7. Diagnostics of Coronal Heating in Solar Active Regions

    Science.gov (United States)

    Fludra, Andrzej; Hornsey, Christopher; Nakariakov, Valery

    2015-04-01

    We aim to develop a diagnostic method for the coronal heating mechanism in active region loops. Observational constraints on coronal heating models have been sought using measurements in the X-ray and EUV wavelengths. Statistical analysis, using EUV emission from many active regions, was done by Fludra and Ireland (2008) who studied power-law relationships between active region integrated magnetic flux and emission line intensities. A subsequent study by Fludra and Warren (2010) for the first time compared fully resolved images in an EUV spectral line of OV 63.0 nm with the photospheric magnetic field, leading to the identification of a dominant, ubiquitous variable component of the transition region EUV emission and a discovery of a steady basal heating, and deriving the dependence of the basal heating rate on the photospheric magnetic flux density. In this study, we compare models of single coronal loops with EUV observations. We assess to what degree observations of individual coronal loops made in the EUV range are capable of providing constraints on the heating mechanism. We model the coronal magnetic field in an active region using an NLFF extrapolation code applied to a photospheric vector magnetogram from SDO/HMI and select several loops that match an SDO/AIA 171 image of the same active region. We then model the plasma in these loops using a 1D hydrostatic code capable of applying an arbitrary heating rate as a function of magnetic field strength along the loop. From the plasma parameters derived from this model, we calculate the EUV emission along the loop in AIA 171 and 335 bands, and in pure spectral lines of Fe IX 17.1 nm and Fe XVI 33.5 nm. We use different spatial distributions of the heating function: concentrated near the loop top, uniform and concentrated near the footpoints, and investigate their effect on the modelled EUV intensities. We find a diagnostics based on the dependence of the total loop intensity on the shape of the heating function

  8. Estudio retrospectivo de las fractures pertrocantéreas de fémur. Análisis del posicionamiento del tornillo cefálico en el tratamiento con clavo endomedular

    OpenAIRE

    Aguilar Garcia, Marc

    2011-01-01

    La fixació interna de les fractures pertrocantériques es una de les intervencions quirúrgiques més freqüents en Traumatologia. És precisament en les fractures més conminutes i inestables en les que el sistema de fixació i la seva correcta col·locació té major importància per evitar, en la major mesura possible, els desplaçaments secundaris de la fractura. El propòsit d'aquest treball és realitzar una revisió clínica quirúrgica d'aquestes fractures per demostrar el valor predictiu que tenen so...

  9. Pitiriasis liquenoide: estudio retrospectivo clínico epidemiológico de 49 pacientes pediátricos Pityriasis lichenoides: a retrospective clinical and epidemiological study of 49 pediatric patients

    Directory of Open Access Journals (Sweden)

    GP Sciancalepore

    Full Text Available La pitiriasis liquenoide (PL, entidad pápulo-escamosa, afecta principalmente a niños. Presenta una forma aguda, "pitiriasis liquenoide y varioliforme aguda" (PLEVA y otra crónica, la pitiriasis liquenoide crónica (PLC. Objetivo: describir las características de pacientes con diagnóstico clínico e histopatológico de PL. Comparar nuestros resultados con los hallados en la bibliografía. Materiales y Métodos: historias clínicas e informes anátomo-patológicos de 49 pacientes que consultaron entre marzo de 2000 a marzo de 2011. Se analizaron los datos obtenidos mediante el programa SPSS 11.5. Resultados: de 49 pacientes con PL, 17 presentaron PLEVA y 32 PLC. El promedio de edad de inicio de PLEVA fue de 6 años y de 10 años para PLC. Predominó el sexo masculino en PLEVA. Las formas generalizadas parecieran ser las predominantes. Las lesiones más frecuentemente halladas fueron: pápulas y pápulas eritematosas en PLEVA, escamas en PLC y las máculas hipocrómicas como discromía residual. 14 de 49 pacientes mostraron asociaciones mórbidas. Conclusiones: la PL puede ser dividida en aguda y crónica, a pesar de existir ambas clases de lesiones en un mismo paciente. PLEVA se presentó a edades más tempranas, predominando en varones. De los pacientes que presentaron co-morbilidades, la mayoría comprometía la inmunidad.Background: the pityriasis lichenoides (PL, a papulosquamous disease, affects mostly children. Present an acute form, pytiriasis lichenoides et varioliformis acute (PLEVA and other chronic, chronic lichenoid pytiriasis (PLC. Objetive: to describe the caracheristics of patients with clinic and histopathological diagnosis of PL. Compare our results with those found in the literature. Materials and Methods: clinical records and pathology reports of 49 patients who consulted between March 2000 and March 2011. Data were analyzed using SPSS 11.5. Results: of 49 patients with PL, 17 presented PLEVA and 32 PLC. The average age of onset of PLEVA was 6 years and 10 years for PLC. Males predominate in PLEVA. The lesions most frequently found were: papules and erythematous papules in PLEVA, scales in PLC and hypocromic macules as residual dyschromia. 14 of 49 patients showed morbid associations. Conclusions: the PL can be divided into acute and chronic forms, despite the existence of both types of lesions in the same patient. PLEVA was presented at younger age, predominantly in males. From the patients who had co-morbidities, the most of them, compromised immunity.

  10. Cambio en la clasificación macroscópica de la apendicitis. ¿Tiene algún impacto? Estudio retrospectivo en un Hospital Universitario Pediátrico

    Directory of Open Access Journals (Sweden)

    Sergio David Castañeda Espinosa

    2015-04-01

    Conclusión. El cambio en la clasificación macroscópica y el aportar la nueva definición sobre apendicitis perforada ha logrado disminuir la estancia hospitalaria y la cantidad de antibióticos utilizados sin una repercusión significativa en la tasa de complicaciones.

  11. Retraso diagnóstico y resistencias primarias en VIH. Estudio observacional, descriptivo, retrospectivo de una cohorte de pacientes de un hospital de referencia en Salamanca, España

    OpenAIRE

    Monsalve Arteaga, Lía Carolina

    2016-01-01

    Trabajo de Fin de Máster en Enfermedades Tropicales. Curso 2015-2016 [ES]Introducción: Todo diagnóstico tardío conlleva un inicio retardado, e inadecuado por tanto, del tratamiento antirretrovírico (TAR). Se define como “presentación tardía” (PT) cuando el paciente presenta un recuento de linfocitos T CD4(+) inferior a 350 células/µl al diagnóstico o un evento definitorio de Sida. Asimismo, una cifra de CD4(+) inferior a 200 células/µl al diagnóstico y/o la presencia de enfermedad...

  12. 59. Estudio multicéntrico retrospectivo de comparación de dos dosis diferentes de ácido tranexámico en cirugía cardíaca

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    E. Martín

    2012-04-01

    Conclusiones: La pauta de AT del grupo A reduce significativamente el sangrado en las primeras 12 h del postoperatorio frente a la del grupo B, aunque no ha demostrado reducir las necesidades transfusionales.

  13. Correlação entre etiologia e a localização das estenoses de uretra - estudo retrospectivo em pacientes atendidos no CHS/PUC-SP

    Directory of Open Access Journals (Sweden)

    Marcelo Cabral Lamy de Miranda

    2008-07-01

    Full Text Available RESUMO Objetivo: análise retrospectiva dos pacientes que estão no programa de dilatação de uretra do Conjunto Hospitalar de Sorocaba, levando em consideração as principais localizações de estenose de uretra relacionada com suas causas específicas e prevalências, no período de fevereiro de 2002 a abril de 2005. Sujeitos e métodos: este trabalho foi realizado mediante estudo retrospectivo dos prontuários médicos e fichas de cadastramento do programa de dilatação de uretra de 115 pacientes registrados no período de fevereiro de 2002 a abril de 2005. Resultados: neste estudo, os pacientes com estenose de uretra tiveram como média de idade 57,5 anos e 3,33% eram do sexo feminino. Nos pacientes do sexo masculino foram encontrados 49,17% das lesões na uretra anterior, enquanto que 47,5% na uretra posterior. As principais localidades de estenose notificadas foram: meato, com 31 casos (25,8%; uretra prostática, com 23 casos (19,1%; colo, com 22 casos (18,33%; fossa navicular, com 21 casos (17,5%; uretra bulbar, com 13 casos (10,8%; uretra peniana, com 6 casos (5%; uretra feminina, com 4 casos (3,33%.

  14. El exilio como campo de estudios en ciencias sociales: análisis bibliométrico

    Directory of Open Access Journals (Sweden)

    José Hernando Ávila-Toscano

    2017-01-01

    Full Text Available Objetivo: formular una revisión bibliométrica de producciones científicas cuyo tema central de análisis es el exilio, con el fin de comprender el panorama de estudio actual en Ciencias Sociales en torno a dicho fenómeno. Método: a través de un diseño bibliométrico descriptivo, retrospectivo, fueron revisados 50 artículos publicados entre 2005 y 2015 en revistas Latinoamericanas. Los documentos se analizaron acorde con el país de producción, la coautoría, las áreas del conocimiento y los términos clave empleados, esto mediante análisis descriptivo y la construcción de grafos de redes. Resultados: sobresalió la Historia como el área de mayor producción frente al exilio, seguida de los estudios literarios y de los de corte sociológico; se observa poca tendencia a producir de forma cooperativa este tipo de trabajos aunque la riqueza temática es amplia.

  15. DISPELLING ILLUSIONS OF REFLECTION: A NEW ANALYSIS OF THE 2007 MAY 19 CORONAL 'WAVE' EVENT

    International Nuclear Information System (INIS)

    Attrill, Gemma D. R.

    2010-01-01

    A new analysis of the 2007 May 19 coronal wave-coronal mass ejection-dimmings event is offered employing base difference extreme-ultraviolet (EUV) images. Previous work analyzing the coronal wave associated with this event concluded strongly in favor of purely an MHD wave interpretation for the expanding bright front. This conclusion was based to a significant extent on the identification of multiple reflections of the coronal wave front. The analysis presented here shows that the previously identified 'reflections' are actually optical illusions and result from a misinterpretation of the running difference EUV data. The results of this new multiwavelength analysis indicate that two coronal wave fronts actually developed during the eruption. This new analysis has implications for our understanding of diffuse coronal waves and questions the validity of the analysis and conclusions reached in previous studies.

  16. Consecuencias del bullying homofóbico retrospectivo y los factores psicosociales en el bienestar psicológico de sujetos LGB

    OpenAIRE

    Marchueta Perez, Aitor

    2014-01-01

    El estudio actual tuvo como principal objetivo analizar si aquellas personas lesbianas, gais y bisexuales (LGB) que sufrieron un evento estresante en la infancia y/o adolescencia, tal como haber sido víctima de acoso escolar por motivo de orientación afectivo-sexual, tiene consecuencias negativas en su bienestar psicológico. Los resultados obtenidos en este estudio, realizado con 119 gais, lesbianas y bisexuales, sugieren que el bullying sufrido en el pasado influye en el bienestar psicológic...

  17. Estudios sobre Plantas Andinas, X

    Directory of Open Access Journals (Sweden)

    Cuatrecasas José

    1967-09-01

    Full Text Available Durante la preparación del género Baccharis para Prima Flora Colombiana tuve que estudiar gran número de especies andinas, tropicales y extratropicales de fuera de Colombia; el objeto principal de tales estudios fue el de tipificar las especies íntimamente relacionadas con las colombianas y establecer su diferenciación taxonómica. La consulta de los tipos específicos y la identificación de gran número de colecciones procedentes de las regiones andinas hasta el sur del continente americano permitió precisar el concepto de bastantes especies y de su área geográfica, al mismo tiempo que el establecimiento de numerosas sinonimias.  La mayor parte de las novedades taxonómicas y de los comentarios derivados de tal estudio va incluída en el texto de las Astereae de Colombia a publicar en breve. El objeto de este artículo es dar a conocer otra parte de las novedades relativas a especies andinas de los países vecinos y describir varias entidades taxonómicas deficientemente conocidas, incorporando a su conocimiento los resultados de muchas disecciones llevadas a cabo en los mencionados estudios.  El trabajo basico para estas notas fue hecho en la Smithsonian Institution; se consultaron también las colecciones de los herbarios europeos de Londres, París, Florencia, Ginebra y Madrid en viaje hecho en otoño de 1963. National Science Foundation de Washington D.C. subvencionó los trabajos.

  18. LOS ESTUDIOS DE POBREZA URBANA

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    Rina De León Herrera

    2007-08-01

    Full Text Available En este artículo se intenta mostrar en forma sucinta la evolución de los estudios de pobreza urbana; se retoma para ello la producción escritural de investigadores que han hecho aportes valiosos sobre la temática en diferentes épocas y espacios geográficos. La información se ha organizado en dos unidades de análisis: la producción escritural en los países desarrollados y en los países en desarrollo.

  19. Esclavizada en los Estudios Poscoloniales

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    Nellys Montenegro De la Hoz

    2014-01-01

    Full Text Available Este ensayo va a centrarse en el análisis de las formas de resis - tencia e identidad esclavizada presentes en Changó, el gran putas de Manuel Zapata Olivella, a través del análisis de los discur - sos hegemónicos y subalternos que hacían parte del sistema de poder, y la intervención de las teorías o estudios poscoloniales que cuestionan dichas perspectivas para redefinir las diferencias de las identidades contradictorias y desarrollar de esta manera literaturas deslindadas de las estructuras ideológicas y hegemónicas.

  20. Coronal pulp biomarker: A lesser known age estimation modality

    Directory of Open Access Journals (Sweden)

    Smrithi D Veera

    2014-01-01

    Full Text Available Introduction: The evolving state of art digital technology currently available is opening new avenues in forensic odontology for age estimation methods which are subject to debate in terms of accuracy and precision. A study was carried to analyze efficacy and practical application for age estimation using digital panoramic radiographs on South Indian population. Aims and Objectives: 1. To study reduction of coronal pulp chamber using Tooth Coronal Index (TCI on panoramic radiographs and correlate with chronologic age. 2. To establish accuracy of digital panoramic radiographs as a simple, non-invasive tool. Materials and Methods: The study illustrates the potential value of a little known aging method. The study groups comprised a total of 100 subjects of both sexes in age range of 20 and 60 years each who were subjected to panoramic radiography. A panoramic radiographic examination using digital panoramic machine was conducted on selected individuals. The TCI was calibrated using AGFA computer software for accuracy and precision. The values obtained were subjected to regression analysis, results calculated and correlated with chronologic age. In the present study a population of known age was studied and subjected to digital panoramic radiographic examination. The correlation between reduction of coronal pulp cavity and chronological age was examined. TCI was computed for each tooth and regressed on real age. Statistical Analysis Used: Pearson correlation co-efficient was used to find the significance of relationship between age and TCI. Regression analysis has been used for predicting age using TCI for premolar and molar. Inaccuracy and bias have been determined to assess the precision of prediction equations. Results and Conclusion: Prediction potential of TCI comes down for ages above 50 years and is comfortably good below 50 years without much difference between premolars and molars. This study demonstrates the potential value of TCI for age

  1. Expansion and broadening of coronal loop transients: A theoretical explanation

    International Nuclear Information System (INIS)

    Mouschovias, T.C.; Poland, A.I.

    1978-01-01

    We explore the consequences of the assumption that a coronal loop transient (observed by the white-light coronagraph aboard Skylab) is a twisted rope of magnetic field lines expanding and broadening in the background coronal plasma and magnetic field. We show that the expansion (i.e., the outward motion of the loop top) can be accounted for by the azimuthal component of the field, B/sub az/; the observed broadening of the loop as it moves outward can be accounted for by the longitudinal component of the field, B/sub l/. In order to have a net outward force and at the same time avoid a classicial pinch (sausage) instability, the two components of the field must satisfy the inequality 1.41 B/sub l/>B/sub az/>B/sub l/.We predict that, as the loop rises, the width (h) of its top portion should vary proportionally with the distance (R) from the Sun's center. This is in good agreement with measurements that show hproportionalR/sup 0.8/. Our prediction, that the radius of curvature (R/sub c/) of the top portion of the loop should be proportional to R, differs from the measured variation R/sub c/proportionalR/sup 1.6/. The difference could be accounted for by a drag due to the background coronal field that flattens the loop's top. A statistical study that can test this possibility is suggested. We also calculate the magnetic field within the top section of the loop. It is approximately equal to 1 gauss at R=2 R/sub sun/ and varies somewhat more slowly than R -2 during expansion

  2. ON THE NATURE OF THE SOLAR WIND FROM CORONAL PSEUDOSTREAMERS

    International Nuclear Information System (INIS)

    Wang, Y.-M.; Sheeley, N. R. J.R.; Grappin, R.; Robbrecht, E.

    2012-01-01

    Coronal pseudostreamers, which separate like-polarity coronal holes, do not have current sheet extensions, unlike the familiar helmet streamers that separate opposite-polarity holes. Both types of streamers taper into narrow plasma sheets that are maintained by continual interchange reconnection with the adjacent open magnetic field lines. White-light observations show that pseudostreamers do not emit plasma blobs; this important difference from helmet streamers is due to the convergence of like-polarity field lines above the X-point, which prevents the underlying loops from expanding outward and pinching off. The main component of the pseudostreamer wind has the form of steady outflow along the open field lines rooted just inside the boundaries of the adjacent coronal holes. These flux tubes are characterized by very rapid expansion below the X-point, followed by reconvergence at greater heights. Analysis of an idealized pseudostreamer configuration shows that, as the separation between the underlying holes increases, the X-point rises and the expansion factor f ss at the source surface increases. In situ observations of pseudostreamer crossings indicate wind speeds v ranging from ∼350 to ∼550 km s –1 , with O 7+ /O 6+ ratios that are enhanced compared with those in high-speed streams but substantially lower than in the slow solar wind. Hydrodynamic energy-balance models show that the empirical v-f ss relation overestimates the wind speeds from nonmonotonically expanding flux tubes, particularly when the X-point is located at low heights and f ss is small. We conclude that pseudostreamers produce a 'hybrid' type of outflow that is intermediate between classical slow and fast solar wind.

  3. The Prospect for Detecting Stellar Coronal Mass Ejections

    Science.gov (United States)

    Osten, Rachel A.; Crosley, Michael Kevin

    2018-06-01

    The astrophysical study of mass loss, both steady-state and transient, on the cool half of the HR diagram has implications bothfor the star itself and the conditions created around the star that can be hospitable or inimical to supporting life. Recent results from exoplanet studies show that planets around M dwarfs are exceedingly common, which together with the commonality of M dwarfs in our galaxy make this the dominant mode of star and planet configurations. The closeness of the exoplanets to the parent M star motivate a comprehensive understanding of habitability for these systems. Radio observations provide the most clear signature of accelerated particles and shocks in stars arising as the result of MHD processes in the stellar outer atmosphere. Stellar coronal mass ejections have not been conclusively detected, despite the ubiquity with which their radiative counterparts in an eruptive event (stellar flares) have. I will review some of the different observational methods which have been used and possibly could be used in the future in the stellar case, emphasizing some of the difficulties inherent in such attempts. I will provide a framework for interpreting potential transient stellar mass loss in light of the properties of flares known to occur on magnetically active stars. This uses a physically motivated way to connect the properties of flares and coronal mass ejections and provides a testable hypothesis for observing or constraining transient stellar mass loss. I will describe recent results using radio observations to detect stellar coronal mass ejections, and what those results imply about transient stellar mass loss. I will provide some motivation for what could be learned in this topic from space-based low frequency radio experiments.

  4. The COronal Solar Magnetism Observatory (COSMO) Large Aperture Coronagraph

    Science.gov (United States)

    Tomczyk, Steve; Gallagher, Dennis; Wu, Zhen; Zhang, Haiying; Nelson, Pete; Burkepile, Joan; Kolinksi, Don; Sutherland, Lee

    2013-04-01

    The COSMO is a facility dedicated to observing coronal and chromospheric magnetic fields. It will be located on a mountaintop in the Hawaiian Islands and will replace the current Mauna Loa Solar Observatory (MLSO). COSMO will provide unique observations of the global coronal magnetic fields and its environment to enhance the value of data collected by other observatories on the ground (e.g. SOLIS, BBO NST, Gregor, ATST, EST, Chinese Giant Solar Telescope, NLST, FASR) and in space (e.g. SDO, Hinode, SOHO, GOES, STEREO, Solar-C, Solar Probe+, Solar Orbiter). COSMO will employ a fleet of instruments to cover many aspects of measuring magnetic fields in the solar atmosphere. The dynamics and energy flow in the corona are dominated by magnetic fields. To understand the formation of CMEs, their relation to other forms of solar activity, and their progression out into the solar wind requires measurements of coronal magnetic fields. The large aperture coronagraph, the Chromospheric and Prominence Magnetometer and the K-Coronagraph form the COSMO instrument suite to measure magnetic fields and the polarization brightness of the low corona used to infer electron density. The large aperture coronagraph will employ a 1.5 meter fuse silica singlet lens, birefringent filters, and a spectropolarimeter to cover fields of view of up to 1 degree. It will observe the corona over a wide range of emission lines from 530.3 nm through 1083.0 nm allowing for magnetic field measurements over a wide range of coronal temperatures (e.g. FeXIV at 530.3 nm, Fe X at 637.4 nm, Fe XIII at 1074.7 and 1079.8 nm. These lines are faint and require the very large aperture. NCAR and NSF have provided funding to bring the large aperture coronagraph to a preliminary design review state by the end of 2013. As with all data from Mauna Loa, the data products from COSMO will be available to the community via the Mauna Loa website: http://mlso.hao.ucar.edu

  5. Paraboloidal X-ray telescope mirror for solar coronal spectroscopy

    Science.gov (United States)

    Brown, W. A.; Bruner, E. C., Jr.; Acton, L. W.; Franks, A.; Stedman, M.; Speer, R. J.

    1979-01-01

    The telescope mirror for the X-ray Spectrograph Spectrometer Telescope System is a sixty degree sector of an extreme off-axis paraboloid of revolution. It was designed to focus a coronal region 1 by 10 arc seconds in size on the entrance slit of the spectrometer after reflection from the gold surface. This paper discusses the design, manufacture, and metrology of the mirror, the methods of precision mechanical metrology used to focus the system, and the mounting system which locates the mirror and has proven itself through vibration tests. In addition, the results of reflection efficiency measurements, alignment tolerances, and ray trace analysis of the effects of misalignment are considered.

  6. The Radiation, Interplanetary Shocks, and Coronal Sources (RISCS) Toolset

    Science.gov (United States)

    Zank, G. P.; Spann, James F.

    2014-01-01

    The goal of this project is to serve the needs of space system designers and operators by developing an interplanetary radiation environment model within 10 AU:Radiation, Interplanetary Shocks, and Coronal Sources (RISCS) toolset: (1) The RISCS toolset will provide specific reference environments for space system designers and nowcasting and forecasting capabilities for space system operators; (2) We envision the RISCS toolset providing the spatial and temporal radiation environment external to the Earth's (and other planets') magnetosphere, as well as possessing the modularity to integrate separate applications (apps) that can map to specific magnetosphere locations and/or perform the subsequent radiation transport and dosimetry for a specific target.

  7. Estudo retrospectivo das complicações intra-operatórias na cirurgia de revascularização do miocárdio

    Directory of Open Access Journals (Sweden)

    Ariana Rodrigues Silva Carvalho

    2008-12-01

    Full Text Available As complicações intra-operatórias na cirurgia de revascularização miocárdica (CRM quando reconhecidas previamente podem guiar os cuidados prestados na sala operatória, dando continuidade na Unidade de Terapia Intensiva e durante toda internação. Quando a equipe conhece essas complicações sofridas pelo indivíduo poderá prever e prover cuidados mais específicos na seqüência de sua evolução cirúrgica. O objetivo desse estudo foi investigar a freqüência e tipos de complicações observadas no intra-operatório da CRM. Trata-se de um estudo retrospectivo, descritivo, transversal, baseado em dados secundários, com amostra intencional de 123 sujeitos. A coleta de dados realizou-se por meio do acesso ao banco de dados do Instituto de Moléstias Cardiovasculares do Oeste do Paraná, em Cascavel. Os dados foram analisados no programa computadorizado Statistic, versão 6,0. Os tipos de complicações observadas nesse período foram: cardiovasculares, pulmonares, alteração nos vasos do enxerto e sangramento. Dentre essas, a que obteve maior freqüência foi “alteração nos vasos do enxerto”, em 33 (26,8% casos. As complicações no intra-operatório podem não ser passíveis de prevenção quando consideradas as características individuais de cada sujeito, entretanto, todos os esforços precisam ser direcionados para que o evento, quando ocorrer, seja bem atendido, evitando dessa forma, complicações adicionais maiores.

  8. Fraturas vertebrais em grandes animais: estudo retrospectivo de 39 casos (1987-2002 Vertebral fractures in large animals: retrospective study of 39 cases (1987-2002

    Directory of Open Access Journals (Sweden)

    A.S. Borges

    2003-04-01

    Full Text Available Realizou-se estudo retrospectivo (1987-2002 dos aspectos clínicos das fraturas vertebrais em eqüinos, bovinos, ovinos, caprinos e suínos atendidos no hospital veterinário da FMVZ-Unesp de Botucatu. Todos os casos tiveram confirmação radiográfica ou post-mortem. Segundo a espécie, a ordem de acometimento foi: bovina, eqüina, ovina, caprina e suína. As lesões ocorreram desde os 12 dias de idade até os 10 anos, com maior freqüência até os 12 meses. O segmento torácico foi o mais comprometido seguido dos segmentos lombar, cervical e sacral. As fraturas vertebrais devem fazer parte da lista de diagnósticos diferenciais de animais em decúbito, independente da espécie, sexo ou idade.It was performed a retrospective study (1987-2002 of clinical features of spinal fractures in the equine, bovine, ovine, caprine and swine referred to the Veterinary Hospital - FMVZ-Unesp in Botucatu, SP, Brazil. All the cases were confirmed by necropsy or radiographic evaluation. Bovines were the most affected species, followed by horses, sheep, goats and swines, and lesions occurred from 12 days to 10 years of age, being more frequent up to 12 months of age. Thoracic vertebrae were the most affected, followed by lumbar, cervical and sacral segments. Vertebral fractures should be included for differential diagnosis of recumbent animals, independently on species, sex or age.

  9. Does correction of preoperative coronal imbalance make a difference in outcomes of adult patients with deformity?

    Science.gov (United States)

    Daubs, Michael D; Lenke, Lawrence G; Bridwell, Keith H; Kim, Yongjung J; Hung, Man; Cheh, Gene; Koester, Linda A

    2013-03-15

    Retrospective study with prospectively collected outcomes data. Determine the significance of coronal balance on spinal deformity surgery outcomes. Sagittal balance has been confirmed as an important radiographic parameter correlating with adult deformity treatment outcomes. The significance of coronal balance on functional outcomes is less clear. Eighty-five patients with more than 4 cm of coronal imbalance who underwent reconstructive spinal surgery were evaluated to determine the significance of coronal balance on functional outcomes as measured with the Oswestry Disability Index (ODI) and Scoliosis Research Society outcomes questionnaires. Sixty-two patients had combined coronal (>4 cm) and sagittal imbalance (>5 cm), while 23 patients had coronal imbalance alone. Postoperatively, 85% of patients demonstrated improved coronal balance. The mean improvement in the coronal C7 plumb line was 26 mm for a mean correction of 42%. The mean preoperative sagittal C7 plumb line in patients with combined coronal and sagittal imbalance was 118 mm (range, 50-310 mm) and improved to a mean 49 mm. The mean preoperative and postoperative ODI scores were 42 (range, 0-90) and 27 (range, 0-78), for a mean improvement of 15 (36%) (P = 0.00001; 95% CI, 12-20). The mean Scoliosis Research Society scores improved by 17 points (29%) (P = 0.00). Younger age (P = 0.008) and improvement in sagittal balance (P = 0.014) were positive predictors for improved ODI scores. Improvement in sagittal balance (P = 0.010) was a positive predictor for improved Scoliosis Research Society scores. In patients with combined coronal and sagittal imbalance, improvement in sagittal balance was the most significant predictor for improved ODI scores (P = 0.009). In patients with preoperative coronal imbalance alone, improvement in coronal balance trended toward, but was not a significant predictor for improved ODI (P = 0.092). Sagittal balance improvement is the strongest predictor of improved outcomes in

  10. ON THE FOURIER AND WAVELET ANALYSIS OF CORONAL TIME SERIES

    International Nuclear Information System (INIS)

    Auchère, F.; Froment, C.; Bocchialini, K.; Buchlin, E.; Solomon, J.

    2016-01-01

    Using Fourier and wavelet analysis, we critically re-assess the significance of our detection of periodic pulsations in coronal loops. We show that the proper identification of the frequency dependence and statistical properties of the different components of the power spectra provides a strong argument against the common practice of data detrending, which tends to produce spurious detections around the cut-off frequency of the filter. In addition, the white and red noise models built into the widely used wavelet code of Torrence and Compo cannot, in most cases, adequately represent the power spectra of coronal time series, thus also possibly causing false positives. Both effects suggest that several reports of periodic phenomena should be re-examined. The Torrence and Compo code nonetheless effectively computes rigorous confidence levels if provided with pertinent models of mean power spectra, and we describe the appropriate manner in which to call its core routines. We recall the meaning of the default confidence levels output from the code, and we propose new Monte-Carlo-derived levels that take into account the total number of degrees of freedom in the wavelet spectra. These improvements allow us to confirm that the power peaks that we detected have a very low probability of being caused by noise.

  11. Examining the Properties of Jets in Coronal Holes

    Science.gov (United States)

    Gaulle, Owen; Adams, Mitzi L.; Tennant, A. F.

    2012-01-01

    Data from the Solar Dynamics Observatory (SDO) were used to look for triggers of jets in a coronal hole. It has been proposed that bright points affiliated with the jets are caused by either random collisions between magnetic elements or by magnetic flux emerging from the photosphere; either of which can give rise to magnetic reconnection. Images from the 193AA filter of the Atmospheric Imaging Assembly (AIA) were searched to identify and locate jets. Changes in the line-of-sight magnetic field prior to the time of the jet were sought in data from the Helioseismic Magnetic Imager (HMI). In total we studied 15 different jets that occurred over a two day period starting 2011-02-27 00:00:00 UTC and ending 2011-02-28 23:59:55 UTC. All of the jets were contained within a coronal hole that was close to disk center. Of the 15 that we studied 6 were shown to have an increase of the parameter B2 (where B is the line-of-sight component of the magnetic field), within one hour prior to the creation of the jet and 10 were within 3 hours before the event.

  12. Filament shape versus coronal potential magnetic field structure

    Science.gov (United States)

    Filippov, B.

    2016-01-01

    Solar filament shape in projection on disc depends on the structure of the coronal magnetic field. We calculate the position of polarity inversion lines (PILs) of coronal potential magnetic field at different heights above the photosphere, which compose the magnetic neutral surface, and compare with them the distribution of the filament material in Hα chromospheric images. We found that the most of the filament material is enclosed between two PILs, one at a lower height close to the chromosphere and one at a higher level, which can be considered as a height of the filament spine. Observations of the same filament on the limb by the Solar Terrestrial Relations Observatory spacecraft confirm that the height of the spine is really very close to the value obtained from the PIL and filament border matching. Such matching can be used for filament height estimations in on-disc observations. Filament barbs are housed within protruding sections of the low-level PIL. On the base of simple model, we show that the similarity of the neutral surfaces in potential and non-potential fields with the same sub-photospheric sources is the reason for the found tendency for the filament material to gather near the potential-field neutral surface.

  13. Posterior coronal plating for tibial fractures: technique and advantages

    Directory of Open Access Journals (Sweden)

    Montu Jain

    2014-04-01

    Full Text Available Objective:Tibial shaft fractures are straightforward to treat but when associated with soft tissue injury particularly at the nail entry/plate insertion site or there is significant comminution proximally or a large butterfly fragment/a second split component in the posterior coronal plane, it is a challenge to the treating surgeon. The aim of the present report is to describe the technique of posterior coronal plating in such a scenario and its advantages. Methods:Between July 2008 and June 2011, 12 patients were pro spectively treated by this approach using 4.5 mm broad dynamic compression plates. Results:The time of bony consolidation and full weight bearing averaged 21.7 weeks (range, 16-26 weeks. Patients were followed up for at least 24 months (range, 24-48 months. At 1 year postoper atively, no loss in reduction or alignment was observed. Mean Hospital for Lower Extremity Measurement Functional Score was 72.8 (range, 64-78. All patients were satisfied with their treatment outcomes. Conclusion:Direct posterior approach and fixation using prone position helps to visualise the fracture fragments and provide rigid fixation. The approach is simple and extensile easily, apart from advantages of less soft tissue and hardware problems compared to standard medial or lateral plating. Key words: Tibial fractures; Bone plates; Orthopedic procedures

  14. ON THE OBSERVATION AND SIMULATION OF SOLAR CORONAL TWIN JETS

    Energy Technology Data Exchange (ETDEWEB)

    Liu, Jiajia; Wang, Yuming; Zhang, Quanhao [CAS Key Laboratory of Geospace Environment, School of Earth and Space Sciences, University of Science and Technology of China, NO. 96, Jinzhai Road, Hefei, Anhui 230026 (China); Fang, Fang [Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, 1234 Innovation Drive, Boulder, CO 80303 (United States); McIntosh, Scott W.; Fan, Yuhong [High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307 (United States)

    2016-02-01

    We present the first observation, analysis, and modeling of solar coronal twin jets, which occurred after a preceding jet. Detailed analysis on the kinetics of the preceding jet reveals its blowout-jet nature, which resembles the one studied in Liu et al. However, the erupting process and kinetics of the twin jets appear to be different from the preceding one. Lacking detailed information on the magnetic fields in the twin jet region, we instead use a numerical simulation using a three-dimensional (3D) MHD model as described in Fang et al., and find that in the simulation a pair of twin jets form due to reconnection between the ambient open fields and a highly twisted sigmoidal magnetic flux, which is the outcome of the further evolution of the magnetic fields following the preceding blowout jet. Based on the similarity between the synthesized and observed emission, we propose this mechanism as a possible explanation for the observed twin jets. Combining our observation and simulation, we suggest that with continuous energy transport from the subsurface convection zone into the corona, solar coronal twin jets could be generated in the same fashion addressed above.

  15. Electron acceleration and radiation signatures in loop coronal transients

    International Nuclear Information System (INIS)

    Vlahos, L.; Gergely, T.E.; Papadopoulos, K.

    1982-01-01

    A model for electron aceleration in loop coronal transients is suggested. We propose that in these transients an erupting loop moves away from the solar surface, with a velocity greater than the local Alfven speed, pushing against the overlying magnetic fields and driving a shock in the front of the moving part of the loop. We suggest that lower hybrid waves are excited at the shock front and propagate radially toward the center of the loop with phase velocity along the magnetic field which exceeds the thermal velocity. The lower hybrid waves stochastically accelerate the tail of the electron distribution inside the loop. We discuss how the accelerated electrons are trapped in the moving loop and give a rough estimate of their radiation signature. We find that plasma radiation can explain the power observed in stationary and moving type IV bursts. We discuss some of the conditions under which moving or stationary type IV bursts are expected to be associated with loop coronal transients

  16. SAUSAGE WAVES IN TRANSVERSELY NONUNIFORM MONOLITHIC CORONAL TUBES

    Energy Technology Data Exchange (ETDEWEB)

    Lopin, I. [Ussuriisk astrophysical observatory, Russion Academy of Sciences (Russian Federation); Nagorny, I., E-mail: lopin78@mail.ru [Institute of Automation and Control Processes FEB RAS, Vladivostok (Russian Federation)

    2015-09-10

    We investigate fast sausage waves in a monolithic coronal magnetic tube, modeled as a local density inhomogeneity with a continuous radial profile. This work is a natural extension of our previous results, obtained for a slab loop model for the case of cylindrical geometry. Using Kneser’s oscillating theorem, we provided the criteria for the existence of trapped and leaky wave regimes as a function of the profile features. For a number of density profiles there are only trapped modes for the entire range of longitudinal wave numbers. The phase speed of these modes tends toward the external Alfvén speed in the long wavelength limit. The generalized results were supported by the analytic solution of the wave equation for the specific density profiles. The approximate Wentzel–Kramers–Brillouin solutions allowed us to obtain the desired dispersion relations and to study their properties as a function of the profile parameters. The multicomponent quasi-periodic pulsations in flaring loops, observed on 2001 May 2 and 2002 July 3, are interpreted in terms of the transversely fundamental trapped fast sausage mode with several longitudinal harmonics in a smooth coronal waveguide.

  17. Activity associated with the solar origin of coronal mass ejections

    Science.gov (United States)

    Webb, D. F.; Hundhausen, A. J.

    1987-01-01

    Solar coronal mass ejections (CMEs) observed in 1980 with the HAO Coronagraph/Polarimeter on the Solar Maximum Mission (SMM) satellite are compared with other forms of solar activity that might be physically related to the ejections. The solar phenomena checked and the method of association used were intentionally patterned after those of Munro et al.'s (1979) analysis of mass ejections observed with the Skylab coronagraph to facilitate comparison of the two epochs. Comparison of the results reveals that the types and degree of CME associations are similar near solar activity minimum and at maximum. For both epochs, most CMEs with associations had associated eruptive prominences, and the proportions of association of all types of activity were similar. A high percentage of association between SMM CMEs and X-ray long duration events is also found, in agreement with Skylab results. It is concluded that most CMEs are the result of the destabilization and eruption of a prominence and its overlying coronal structure, or of a magnetic structure capable of supporting a prominence.

  18. Cannabis, possible cardiac deaths and the coroner in Ireland.

    LENUS (Irish Health Repository)

    Tormey, W P

    2012-01-10

    BACKGROUND: The elevated risk of triggering a myocardial infarction by smoking cannabis is limited to the first 2 h after smoking. AIM: To examine the possible role of cannabis in cardiac deaths. CASES AND RESULTS: From 3,193 coroners\\' cases over 2 years, there were 13 cases where the clinical information was compatible with a primary cardiac cause of death. An inquest was held in three cases. Myocardial infarction was the primary cause of death in 54%. Other causes were sudden adult death syndrome, sudden death in epilepsy, and poisoning by alcohol and diazepam. Cannabis was mentioned once only on a death certificate, but not as a cause of death. Blood delta9-tetrahydrocannabinol-carboxylic acid was recorded in one case and in no case was plasma tetrahydrocannabinol (THC) measured. CONCLUSIONS: To attribute sudden cardiac death to cannabis, plasma THC should be measured in the toxicology screen in coroners\\' cases where urine cannabinoids are positive. A positive urine cannabinoids immunoassay alone is insufficient evidence in the linkage of acute cardiac death and cannabis.

  19. ON THE FOURIER AND WAVELET ANALYSIS OF CORONAL TIME SERIES

    Energy Technology Data Exchange (ETDEWEB)

    Auchère, F.; Froment, C.; Bocchialini, K.; Buchlin, E.; Solomon, J., E-mail: frederic.auchere@ias.u-psud.fr [Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Sud, Université Paris-Saclay, Bât. 121, F-91405 Orsay (France)

    2016-07-10

    Using Fourier and wavelet analysis, we critically re-assess the significance of our detection of periodic pulsations in coronal loops. We show that the proper identification of the frequency dependence and statistical properties of the different components of the power spectra provides a strong argument against the common practice of data detrending, which tends to produce spurious detections around the cut-off frequency of the filter. In addition, the white and red noise models built into the widely used wavelet code of Torrence and Compo cannot, in most cases, adequately represent the power spectra of coronal time series, thus also possibly causing false positives. Both effects suggest that several reports of periodic phenomena should be re-examined. The Torrence and Compo code nonetheless effectively computes rigorous confidence levels if provided with pertinent models of mean power spectra, and we describe the appropriate manner in which to call its core routines. We recall the meaning of the default confidence levels output from the code, and we propose new Monte-Carlo-derived levels that take into account the total number of degrees of freedom in the wavelet spectra. These improvements allow us to confirm that the power peaks that we detected have a very low probability of being caused by noise.

  20. On the Occurrence of Thermal Nonequilibrium in Coronal Loops

    Science.gov (United States)

    Froment, C.; Auchère, F.; Mikić, Z.; Aulanier, G.; Bocchialini, K.; Buchlin, E.; Solomon, J.; Soubrié, E.

    2018-03-01

    Long-period EUV pulsations, recently discovered to be common in active regions, are understood to be the coronal manifestation of thermal nonequilibrium (TNE). The active regions previously studied with EIT/Solar and Heliospheric Observatory and AIA/SDO indicated that long-period intensity pulsations are localized in only one or two loop bundles. The basic idea of this study is to understand why. For this purpose, we tested the response of different loop systems, using different magnetic configurations, to different stratifications and strengths of the heating. We present an extensive parameter-space study using 1D hydrodynamic simulations (1020 in total) and conclude that the occurrence of TNE requires specific combinations of parameters. Our study shows that the TNE cycles are confined to specific ranges in parameter space. This naturally explains why only some loops undergo constant periodic pulsations over several days: since the loop geometry and the heating properties generally vary from one loop to another in an active region, only the ones in which these parameters are compatible exhibit TNE cycles. Furthermore, these parameters (heating and geometry) are likely to vary significantly over the duration of a cycle, which potentially limits the possibilities of periodic behavior. This study also confirms that long-period intensity pulsations and coronal rain are two aspects of the same phenomenon: both phenomena can occur for similar heating conditions and can appear simultaneously in the simulations.

  1. Steady three-fluid coronal expansion for nonspherical geometries

    International Nuclear Information System (INIS)

    Joselyn, J.; Holzer, T.E.

    1978-01-01

    A steady three-fluid model of the solar coronal expansionk in which 4 He ++ ions (alphas) are treated as a nonminor species, is developed for nonspherically symmetric flow geometries of the general sort thought to be characteristic of coronal holes. It is found that the very high mass fluxes in the low corona, which are associated with rapidly diverging flow geometries, lead to a locally enhanced frictional coupling between protons and alphas and consequently to a significant reduction of the He/H abundance ratio in the lower corona from that normally predicted by multifluid models. In the models considered, the frictional drag on the protons by the alphas (a process neglected in most studies) is found to play an important role near the sun. Heavy ions, other than alphas, are treated as minor species and are seen to exhibit varying responses to the rapidly diverging flow geometries, depending on the ion mass and charge. As for the protons, the frictional effect of the alphas on the heavier ions is found to be significant in the models considered

  2. AN MHD AVALANCHE IN A MULTI-THREADED CORONAL LOOP

    Energy Technology Data Exchange (ETDEWEB)

    Hood, A. W.; Cargill, P. J.; Tam, K. V. [School of Mathematics and Statistics, University of St Andrews, St Andrews, Fife, KY16 9SS (United Kingdom); Browning, P. K., E-mail: awh@st-andrews.ac.uk [School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester, M13 9PL (United Kingdom)

    2016-01-20

    For the first time, we demonstrate how an MHD avalanche might occur in a multithreaded coronal loop. Considering 23 non-potential magnetic threads within a loop, we use 3D MHD simulations to show that only one thread needs to be unstable in order to start an avalanche even when the others are below marginal stability. This has significant implications for coronal heating in that it provides for energy dissipation with a trigger mechanism. The instability of the unstable thread follows the evolution determined in many earlier investigations. However, once one stable thread is disrupted, it coalesces with a neighboring thread and this process disrupts other nearby threads. Coalescence with these disrupted threads then occurs leading to the disruption of yet more threads as the avalanche develops. Magnetic energy is released in discrete bursts as the surrounding stable threads are disrupted. The volume integrated heating, as a function of time, shows short spikes suggesting that the temporal form of the heating is more like that of nanoflares than of constant heating.

  3. Coronal Flux Rope Catastrophe Associated With Internal Energy Release

    Science.gov (United States)

    Zhuang, Bin; Hu, Youqiu; Wang, Yuming; Zhang, Quanhao; Liu, Rui; Gou, Tingyu; Shen, Chenglong

    2018-04-01

    Magnetic energy during the catastrophe was predominantly studied by the previous catastrophe works since it is believed to be the main energy supplier for the solar eruptions. However, the contribution of other types of energies during the catastrophe cannot be neglected. This paper studies the catastrophe of the coronal flux rope system in the solar wind background, with emphasis on the transformation of different types of energies during the catastrophe. The coronal flux rope is characterized by its axial and poloidal magnetic fluxes and total mass. It is shown that a catastrophe can be triggered by not only an increase but also a decrease of the axial magnetic flux. Moreover, the internal energy of the rope is found to be released during the catastrophe so as to provide energy for the upward eruption of the flux rope. As far as the magnetic energy is concerned, it provides only part of the energy release, or even increases during the catastrophe, so the internal energy may act as the dominant or even the unique energy supplier during the catastrophe.

  4. FORECASTING A CORONAL MASS EJECTION'S ALTERED TRAJECTORY: ForeCAT

    International Nuclear Information System (INIS)

    Kay, C.; Opher, M.; Evans, R. M.

    2013-01-01

    To predict whether a coronal mass ejection (CME) will impact Earth, the effects of the background on the CME's trajectory must be taken into account. We develop a model, ForeCAT (Forecasting a CME's Altered Trajectory), of CME deflection due to magnetic forces. ForeCAT includes CME expansion, a three-part propagation model, and the effects of drag on the CME's deflection. Given the background solar wind conditions, the launch site of the CME, and the properties of the CME (mass, final propagation speed, initial radius, and initial magnetic strength), ForeCAT predicts the deflection of the CME. Two different magnetic backgrounds are considered: a scaled background based on type II radio burst profiles and a potential field source surface (PFSS) background. For a scaled background where the CME is launched from an active region located between a coronal hole and streamer region, the strong magnetic gradients cause a deflection of 8.°1 in latitude and 26.°4 in longitude for a 10 15 g CME propagating out to 1 AU. Using the PFSS background, which captures the variation of the streamer belt (SB) position with height, leads to a deflection of 1.°6 in latitude and 4.°1 in longitude for the control case. Varying the CME's input parameters within observed ranges leads to the majority of CMEs reaching the SB within the first few solar radii. For these specific backgrounds, the SB acts like a potential well that forces the CME into an equilibrium angular position

  5. Determining coronal electron temperatures from observations with UVCS/SOHO

    Science.gov (United States)

    Fineschi, S.; Esser, R.; Habbal, S. R.; Karovska, M.; Romoli, M.; Strachan, L.; Kohl, J. L.; Huber, M. C. E.

    1995-01-01

    The electron temperature is a fundamental physical parameter of the coronal plasma. Currently, there are no direct measurements of this quantity in the extended corona. Observations with the Ultraviolet Coronagraph Spectrometer (UVCS) aboard the upcoming Solar and Heliospheric Observatory (SOHO) mission can provide the most direct determination of the electron kinetic temperature (or, more precisely, the electron velocity distribution along the line of sight). This measurement is based on the observation of the Thomson-scattered Lyman alpha (Ly-alpha) profile. This observation is made particularly challenging by the fact that the integrated intensity of the electron-scattered Ly-alpha line is about 10(exp 3) times fainter than that of the resonantly-scattered Ly-alpha component. In addition, the former is distributed across 50 A (FWHM), unlike the latter that is concentrated in 1 A. These facts impose stringent requirements on the stray-light rejection properties of the coronagraph/spectrometer, and in particular on the requirements for the grating. We make use of laboratory measurements of the UVCS Ly-alpha grating stray-light, and of simulated electron-scattered Ly-alpha profiles to estimate the expected confidence levels of electron temperature determination. Models of different structures typical of the corona (e.g., streamers, coronal holes) are used for this parameter study.

  6. AN IMAGING STUDY OF A COMPLEX SOLAR CORONAL RADIO ERUPTION

    Energy Technology Data Exchange (ETDEWEB)

    Feng, S. W.; Chen, Y.; Song, H. Q.; Wang, B.; Kong, X. L., E-mail: yaochen@sdu.edu.cn [Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, and Institute of Space Sciences, Shandong University, Weihai, Shandong 264209 (China)

    2016-08-10

    Solar coronal radio bursts are enhanced radio emission excited by energetic electrons accelerated during solar eruptions. Studying these bursts is important for investigating the origin and physical mechanism of energetic particles and further diagnosing coronal parameters. Earlier studies suffered from a lack of simultaneous high-quality imaging data of the radio burst and the eruptive structure in the inner corona. Here we present a study on a complex solar radio eruption consisting of a type II burst and three reversely drifting type III bursts, using simultaneous EUV and radio imaging data. It is found that the type II burst is closely associated with a propagating and evolving CME-driven EUV shock structure, originated initially at the northern shock flank and later transferred to the top part of the shock. This source transfer is coincident with the presence of shock decay and enhancing signatures observed at the corresponding side of the EUV front. The electron energy accelerated by the shock at the flank is estimated to be ∼0.3 c by examining the imaging data of the fast-drifting herringbone structure of the type II burst. The reverse-drifting type III sources are found to be within the ejecta and correlated with a likely reconnection event therein. The implications for further observational studies and relevant space weather forecasting techniques are discussed.

  7. On the Observation and Simulation of Solar Coronal Twin Jets

    Science.gov (United States)

    Liu, Jiajia; Fang, Fang; Wang, Yuming; McIntosh, Scott W.; Fan, Yuhong; Zhang, Quanhao

    2016-02-01

    We present the first observation, analysis, and modeling of solar coronal twin jets, which occurred after a preceding jet. Detailed analysis on the kinetics of the preceding jet reveals its blowout-jet nature, which resembles the one studied in Liu et al. However, the erupting process and kinetics of the twin jets appear to be different from the preceding one. Lacking detailed information on the magnetic fields in the twin jet region, we instead use a numerical simulation using a three-dimensional (3D) MHD model as described in Fang et al., and find that in the simulation a pair of twin jets form due to reconnection between the ambient open fields and a highly twisted sigmoidal magnetic flux, which is the outcome of the further evolution of the magnetic fields following the preceding blowout jet. Based on the similarity between the synthesized and observed emission, we propose this mechanism as a possible explanation for the observed twin jets. Combining our observation and simulation, we suggest that with continuous energy transport from the subsurface convection zone into the corona, solar coronal twin jets could be generated in the same fashion addressed above.

  8. Cannabis, possible cardiac deaths and the coroner in Ireland.

    Science.gov (United States)

    Tormey, W P

    2012-12-01

    The elevated risk of triggering a myocardial infarction by smoking cannabis is limited to the first 2 h after smoking. To examine the possible role of cannabis in cardiac deaths. CASES AND RESULTS: From 3,193 coroners' cases over 2 years, there were 13 cases where the clinical information was compatible with a primary cardiac cause of death. An inquest was held in three cases. Myocardial infarction was the primary cause of death in 54%. Other causes were sudden adult death syndrome, sudden death in epilepsy, and poisoning by alcohol and diazepam. Cannabis was mentioned once only on a death certificate, but not as a cause of death. Blood delta9-tetrahydrocannabinol-carboxylic acid was recorded in one case and in no case was plasma tetrahydrocannabinol (THC) measured. To attribute sudden cardiac death to cannabis, plasma THC should be measured in the toxicology screen in coroners' cases where urine cannabinoids are positive. A positive urine cannabinoids immunoassay alone is insufficient evidence in the linkage of acute cardiac death and cannabis.

  9. Global Energetics in Solar Flares and Coronal Mass Ejections

    Science.gov (United States)

    Aschwanden, Markus J.

    2017-08-01

    We present a statistical study of the energetics of coronal mass ejections (CME) and compare it with the magnetic, thermal, and nonthermal energy dissipated in flares. The physical parameters of CME speeds, mass, and kinetic energies are determined with two different independent methods, i.e., the traditional white-light scattering method using LASCO/SOHO data, and the EUV dimming method using AIA/SDO data. We analyze all 860 GOES M- and X-class flare events observed during the first 7 years (2010-2016) of the SDO mission. The new ingredients of our CME modeling includes: (1) CME geometry in terms of a self-similar adiabatic expansion, (2) DEM analysis of CME mass over entire coronal temperature range, (3) deceleration of CME due to gravity force which controls the kinetic and potentail CME energy as a function of time, (4) the critical speed that controls eruptive and confined CMEs, (5) the relationship between the center-of-mass motion during EUV dimming and the leading edge motion observed in white-light coronagraphs. Novel results are: (1) Physical parameters obtained from both the EUV dimming and white-light method can be reconciled; (2) the equi-partition of CME kinetic and thermal flare energy; (3) the Rosner-Tucker-Vaiana scaling law. We find that the two methods in EUV and white-light wavelengths are highly complementary and yield more complete models than each method alone.

  10. THE RELATION BETWEEN EIT WAVES AND CORONAL MASS EJECTIONS

    International Nuclear Information System (INIS)

    Chen, P. F.

    2009-01-01

    More and more evidence indicates that 'EIT waves' are strongly related to coronal mass ejections (CMEs). However, it is still not clear how the two phenomena are related to each other. We investigate a CME event on 1997 September 9, which was well observed by both the EUV Imaging Telescope (EIT) and the high-cadence Mark-III K-Coronameter at Mauna Loa Solar Observatory, and compare the spatial relation between the 'EIT wave' fronts and the CME leading loops. It is found that 'EIT wave' fronts are cospatial with the CME leading loops, and the expanding EUV dimmings are cospatial with the CME cavity. It is also found that the CME stopped near the boundary of a coronal hole, a feature common to observations of 'EIT waves'. It is suggested that 'EIT waves'/dimmings are the EUV counterparts of the CME leading loop/cavity, based on which we propose that, as in the case of 'EIT waves', CME leading loops are apparently moving density enhancements that are generated by successive stretching (or opening-up) of magnetic loops.

  11. Why fast solar wind originates from slowly expanding coronal flux tubes

    International Nuclear Information System (INIS)

    Wang, Y.M.; Sheeley, N.R. Jr.

    1991-01-01

    Empirical studies indicate that the solar wind speed at earth is inversely correlated with the divergence rate of the coronal magnetic field. It is shown that this result is consistent with simple wind acceleration models involving Alfven waves, provided that the wave energy flux at the coronal base is taken to be roughly constant within open field regions. 9 refs

  12. Assessment of Coronal Radiographic Parameters of the Spine in the Treatment of Adolescent Idiopathic Scoliosis.

    Science.gov (United States)

    Karami, Mohsen; Maleki, Arash; Mazda, Keyvan

    2016-10-01

    To determine the most important preoperative factors that affect postoperative coronal parameters of scoliotic curves. All Adolescent Idiopathic Scoliosis (AIS) patients included in the study were classified according to Lenke and King Classification. The fusion levels were selected according to the rigidity of the existing curves (correction less than 50%), tilt of T1 and shoulders, sagittal angle of the curves and with considering stable and neutral end vertebra. The radiographic coronal parameters: shoulders tilt angle, iliolumbar angle and coronal balance were measured in all patients before, after, and in the last follow-up visit. One hundred twenty patients after mean of 25 months follow-up (18-40 months) were included in the study. Before operation, abnormal coronal balance (more than 2 cm shift) was noticed in 46 patents (38%) and in the last visit, was noted in 22 patients (18%). Multivariate regression analysis revealed a significant predictive value of the preoperative coronal balance on the last visit coronal balance ( P value=0.01). Preoperative coronal balance is very important to make a balanced spine after surgery. Other parameters like Lenke classification or main thoracic overcorrection did not affect postoperative coronal decompensation.

  13. Multidetector CT enteroclysis: comparison of the reading performance for axial and coronal views

    International Nuclear Information System (INIS)

    Schmidt, Sabine; Chalaron, Marc; Schnyder, Pierre; Denys, Alban; Chevallier, Patrick; Bessoud, Bertrand; Verdun, Francis R.; Frascarolo, Philippe

    2005-01-01

    The purpose of this study was to compare the diagnostic performance of axial and coronal views in multidetector CT enteroclysis (MDCTE). We retrospectively evaluated 48 patients with pathological correlation investigated by MDCTE for small bowel disorders. After nasojejunal administration of 2 l of 5% methylcellulose axial arterial and venous acquisition of MDCTE was followed by coronal reconstructions using equal slice thicknesses of 2.5 mm with 2 mm increments. Spatial resolution of both planes was evaluated by phantom. Three radiologists independently read axial and coronal images concerning 12 pathological features. The interobserver agreement and time of reading was calculated. Sensitivity and specificity resulted from comparison with histopathology (n=39) or follow-up (n=9). Phantom study revealed higher spatial resolution for axial than coronal views, whatever reconstruction interval was used. However, spatial frequency always remained high. Most pathological signs, such as bowel wall thickening (BWT), bowel wall enhancement (BWE) and intraperitoneal fluid (IPF), showed better interobserver agreement on axial than coronal views (BWT: 0.61 vs. 0.44; BWE: 0.56 vs. 0.5; IPF:0.53 vs. 0.43). The Wilcoxon signed-rank test revealed significantly higher sensitivity for axial than coronal views (P=0.0453); the time of reading was significantly shorter for the latter (P=0.0146). The diagnostic value of axial slices is superior to coronal reconstructions despite the reduced data volume and display of the physiological course of bowel loops on the coronal plane. (orig.)

  14. The Fate of Cool Material in the Hot Corona: Solar Prominences and Coronal Rain

    Science.gov (United States)

    Liu, Wei; Antolin, Patrick; Sun, Xudong; Vial, Jean-Claude; Berger, Thomas

    2017-08-01

    As an important chain of the chromosphere-corona mass cycle, some of the million-degree hot coronal mass undergoes a radiative cooling instability and condenses into material at chromospheric or transition-region temperatures in two distinct forms - prominences and coronal rain (some of which eventually falls back to the chromosphere). A quiescent prominence usually consists of numerous long-lasting, filamentary downflow threads, while coronal rain consists of transient mass blobs falling at comparably higher speeds along well-defined paths. It remains puzzling why such material of similar temperatures exhibit contrasting morphologies and behaviors. We report recent SDO/AIA and IRIS observations that suggest different magnetic environments being responsible for such distinctions. Specifically, in a hybrid prominence-coronal rain complex structure, we found that the prominence material is formed and resides near magnetic null points that favor the radiative cooling process and provide possibly a high plasma-beta environment suitable for the existence of meandering prominence threads. As the cool material descends, it turns into coronal rain tied onto low-lying coronal loops in a likely low-beta environment. Such structures resemble to certain extent the so-called coronal spiders or cloud prominences, but the observations reported here provide critical new insights. We will discuss the broad physical implications of these observations for fundamental questions, such as coronal heating and beyond (e.g., in astrophysical and/or laboratory plasma environments).

  15. Characteristics of Low-latitude Coronal Holes near the Maximum of Solar Cycle 24

    DEFF Research Database (Denmark)

    Hofmeister, Stefan J.; Veronig, Astrid; Reiss, Martin A.

    2017-01-01

    We investigate the statistics of 288 low-latitude coronal holes extracted from SDO/AIA-193 filtergrams over the time range of 2011 January 01–2013 December 31. We analyze the distribution of characteristic coronal hole properties, such as the areas, mean AIA-193 intensities, and mean magnetic fie...

  16. Identification of Low Coronal Sources of “Stealth” Coronal Mass Ejections Using New Image Processing Techniques

    Energy Technology Data Exchange (ETDEWEB)

    Alzate, Nathalia; Morgan, Huw, E-mail: naa19@aber.ac.uk [Institute of Mathematics, Physics and Computer Science Prifysgol Aberystwyth Ceredigion, Cymru SY23 3BZ (United Kingdom)

    2017-05-10

    Coronal mass ejections (CMEs) are generally associated with low coronal signatures (LCSs), such as flares, filament eruptions, extreme ultraviolet (EUV) waves, or jets. A number of recent studies have reported the existence of stealth CMEs as events without LCSs, possibly due to observational limitations. Our study focuses on a set of 40 stealth CMEs identified from a study by D’Huys et al. New image processing techniques are applied to high-cadence, multi-instrument sets of images spanning the onset and propagation time of each of these CMEs to search for possible LCSs. Twenty-three of these events are identified as small, low-mass, unstructured blobs or puffs, often occurring in the aftermath of a large CME, but associated with LCSs such as small flares, jets, or filament eruptions. Of the larger CMEs, seven are associated with jets and eight with filament eruptions. Several of these filament eruptions are different from the standard model of an erupting filament/flux tube in that they are eruptions of large, faint flux tubes that seem to exist at large heights for a long time prior to their slow eruption. For two of these events, we see an eruption in Large Angle Spectrometric Coronagraph C2 images and the consequent changes at the bottom edge of the eruption in EUV images. All 40 events in our study are associated with some form of LCS. We conclude that stealth CMEs arise from observational and processing limitations.

  17. Reconstructed coronal views of CT and isotopic images of the pancreas

    International Nuclear Information System (INIS)

    Kasuga, Toshio; Kobayashi, Toshio; Nakanishi, Fumiko

    1980-01-01

    To compare functional images of the pancreas by scintigraphy with morphological views of the pancreas by CT, CT coronal views of the pancreas were reconstructed. As CT coronal views were reconstructed from the routine scanning, there was a problem in longitudinal spatial resolution. However, almost satisfactory total images of the pancreas were obtained by improving images adequately. In 27 patients whose diseases had been confirmed, it was easy to compare pancreatic scintigrams with pancreatic CT images by using reconstructed CT coronal views, and information which had not been obtained by original CT images could be obtained by using reconstructed CT coronal views. Especially, defects on pancreatic images and the shape of pancreas which had not been visualized clearly by scintigraphy alone could be visualized by using reconstructed CT coronal views of the pancreas. (Tsunoda, M.)

  18. An observationally-driven kinetic approach to coronal heating

    Science.gov (United States)

    Moraitis, K.; Toutountzi, A.; Isliker, H.; Georgoulis, M.; Vlahos, L.; Chintzoglou, G.

    2016-11-01

    Aims: Coronal heating through the explosive release of magnetic energy remains an open problem in solar physics. Recent hydrodynamical models attempt an investigation by placing swarms of "nanoflares" at random sites and times in modeled one-dimensional coronal loops. We investigate the problem in three dimensions, using extrapolated coronal magnetic fields of observed solar active regions. Methods: We applied a nonlinear force-free field extrapolation above an observed photospheric magnetogram of NOAA active region (AR) 11 158. We then determined the locations, energy contents, and volumes of "unstable" areas, namely areas prone to releasing magnetic energy due to locally accumulated electric current density. Statistical distributions of these volumes and their fractal dimension are inferred, investigating also their dependence on spatial resolution. Further adopting a simple resistivity model, we inferred the properties of the fractally distributed electric fields in these volumes. Next, we monitored the evolution of 105 particles (electrons and ions) obeying an initial Maxwellian distribution with a temperature of 10 eV, by following their trajectories and energization when subjected to the resulting electric fields. For computational convenience, the length element of the magnetic-field extrapolation is 1 arcsec, or 725 km, much coarser than the particles' collisional mean free path in the low corona (0.1-1 km). Results: The presence of collisions traps the bulk of the plasma around the unstable volumes, or current sheets (UCS), with only a tail of the distribution gaining substantial energy. Assuming that the distance between UCS is similar to the collisional mean free path we find that the low active-region corona is heated to 100-200 eV, corresponding to temperatures exceeding 2 MK, within tens of seconds for electrons and thousands of seconds for ions. Conclusions: Fractally distributed, nanoflare-triggening fragmented UCS in the active-region corona can

  19. Evidence of thermal conduction depression in hot coronal loops

    Science.gov (United States)

    Wang, Tongjiang; Ofman, Leon; Sun, Xudong; Provornikova, Elena; Davila, Joseph

    2015-08-01

    Slow magnetoacoustic waves were first detected in hot (>6 MK) flare loops by the SOHO/SUMER spectrometer as Doppler shift oscillations in Fe XIX and Fe XXI lines. These oscillations are identified as standing slow-mode waves because the estimated phase speeds are close to the sound speed in the loop and some cases show a quarter period phase shift between velocity and intensity oscillations. The observed very rapid excitation and damping of standing slow mode waves have been studied by many authors using theories and numerical simulations, however, the exact mechanisms remain not well understood. Recently, flare-induced longitudinal intensity oscillations in hot post-flare loops have been detected by SDO/AIA. These oscillations have the similar physical properties as SUMER loop oscillations, and have been interpreted as the slow-mode waves. The multi-wavelength AIA observations with high spatio-temporal resolution and wide temperature coverage allow us to explore the wave excitation and damping mechanisms with an unprecedented detail to develope new coronal seismology. In this paper, we present accurate measurements of the effective adiabatic index (γeff) in the hot plasma from the electron temperature and density wave signals of a flare-induced longitudinal wave event using SDO/AIA data. Our results strikingly and clearly reveal that thermal conduction is highly depressed in hot (˜10 MK) post-flare loops and suggest that the compressive viscosity is the dominant wave damping mechanism which allows determination of the viscosity coefficient from the observables by coronal seismology. This new finding challenges our current understanding of thermal energy transport in solar and stellar flares, and may provide an alternative explanation of long-duration events and enhance our understand of coronal heating mechanism. We will discuss our results based on non-ideal MHD theory and simulations. We will also discuss the flare trigger mechanism based on magnetic topology

  20. 77 FR 24537 - Draft Standards and Best Practices for Interaction Between Medical Examiner/Coroner and Organ and...

    Science.gov (United States)

    2012-04-24

    ... Best Practices for Interaction Between Medical Examiner/Coroner and Organ and Tissue Procurement... Committee Standards and Best Practices for Interaction Between Medical Examiner/Coroner Offices and Organ... coroner/medical examiner office representatives, law enforcement agencies, organizations, and all other...

  1. Enxerto dermoadiposo em cavidades anoftálmicas secundárias: estudo retrospectivo e revisão da literatura

    Directory of Open Access Journals (Sweden)

    Silvia Narikawa

    2011-12-01

    Full Text Available OBJETIVO: Avaliar o uso do enxerto dermoadiposo no tratamento da cavidade anoftálmica. MÉTODOS: Estudo retrospectivo, do qual participaram 28 portadores de cavidade anoftálmica secundária, tratados com enxerto dermoadiposo. Os dados avaliados foram: idade, sexo, motivo da primeira cirurgia, tipo de cavidade, razão da opção pelo enxerto dermoadiposo, resultados e complicações. Os dados foram analisados segundo a frequência de ocorrência. RESULTADOS: dos 28 pacientes analisados, 19 (67,8% eram do sexo masculino, 46,4% deles apresentando de 40 a 60 anos de idade. A principal causa da perda do olho foi o trauma (7 casos - 25,0%. A cavidade onde mais se empregou o enxerto dermoadiposo foi a do tipo III (32,1%. Como primeira cirurgia, a evisceração havia sido realizada em 13 casos, a enucleação em 11 e o enxerto de pele em dois pacientes e em outros dois, não havia informação sobre a primeira cirurgia a que haviam sido submetidos. A opção pelo enxerto dermoadiposo foi feita com a finalidade de repor volume na cavidade e, ao mesmo tempo, conseguir maior superfície anterior da cavidade, já que a maioria possuía cavidades contraídas. A maioria dos pacientes (53,6% não apresentou complicações, tendo sido a necrose do enxerto a complicação mais observada (32,1%. O resultado final da cirurgia foi considerado bom em 71,4% dos pacientes e ruim em 7,1%. CONCLUSÃO: O enxerto dermoadiposo é uma técnica cirúrgica simples e de bons resultados para reposição de volume em cavidades anoftálmicas. Os autores estimulam o ensino da mesma nos serviços de treinamento de jovens cirurgiões.

  2. Tratamento artroscópico da instabilidade anterior do ombro: estudo retrospectivo de 159 casos Anterior instability of the shoulder: retrospective study on 159 cases

    Directory of Open Access Journals (Sweden)

    Arnaldo Amado Ferreira Neto

    2011-01-01

    Full Text Available OBJETIVO: Análise dos resultados de 159 pacientes com instabilidade anterior do ombro submetidos ao tratamento artroscópico de janeiro de 2001 a dezembro de 2005. MÉTODOS: Estudo retrospectivo de prontuários com dados completos. RESULTADOS: Em 108 pacientes notou-se a lesão de Bankart e em 62 pacientes a lesão do tipo SLAP estava presente. Utilizou-se em média 2,7 âncoras. Apresentaram complicações 42 casos; 14 tinham dor aos esforços, 12 tinham algum grau de diminuição da rotação externa, 16 apresentaram recidiva. Os pacientes que evoluíram com complicações utilizaram em média 2,5 âncoras, enquanto naqueles sem complicações a média foi de 2,8 (pOBJECTIVE: To analyze the results of 159 patients with anterior instability of the shoulder submitted to arthroscopic treatment from January 2001 to December 2005. METHODS: Retrospective study of complete patient records. RESULTS: In 108 patients the Bankart lesion was found, while in 62 patients, SLAP type lesions were found. An average of 2.7 anchors was used. 42 cases presented complications; 14 had pain on effort, 12 had some degree of reduction of external rotation, and 16 had recorrence. The patients who developed complications used an average of 2.5 anchors, while those without complications used an average of 2.8 anchors (p<0.05. Of the 35 patients with anterior glenoid bone lesion, 8 had recorrence, while of the 124 patients without fractures, 8 had recorrence (p<0.05. Of the 113 patients with first-time traumatic dislocations, 12 developed limitation of external rotation, while in 46 atraumatic cases none developed limitation (p<0.05. Of the patients with SLAP lesion, 11 developed pain, while in the cases without this lesion, only 3 presented pain (p<0.05. CONCLUSION: There were more recurrences (deveria ser plural e recurrences, nao recurrence in cases of anterior glenoid bone lesion. Post-operative pain was more frequent when the lesion type was SLAP. Limitation of

  3. Prevalência de perda precoce de molares decíduos: estudo retrospectivo = Prevalence of early loss of deciduous molars: a retrospective study

    Directory of Open Access Journals (Sweden)

    Alessandro Leite Cavalcanti

    2008-07-01

    Full Text Available Este estudo retrospectivo determinou a prevalência da perda precoce demolares decíduos em pacientes atendidos na clínica de Odontopediatria da Universidade Estadual da Paraíba. Foram examinados 515 prontuários, sendo os dados registrados em um formulário. Foram analisadas as variáveis: gênero, idade, tipo de molar decíduo perdido,arcada dentária (maxilar ou mandibular e lado (direito e esquerdo. Observou-se que a prevalência de perda precoce foi de 15,1%, existindo uma distribuição similar entre os gêneros. Em relação à idade da criança, a maior freqüência de perda acometeu pacientescom sete anos (32,1%. Houve distribuição equitativa da perda dentária entre as arcadas superior e inferior, com 43,6% cada uma, sendo o lado esquerdo o mais acometido (41%. O segundo molar superior esquerdo foi o mais acometido (17,9%, seguido do primeiromolar decíduo superior direito (16,1%. Pode-se concluir que a prevalência de perda precoce foi baixa e que os molares decíduos superiores foram os dentes mais comumente perdidos.This retrospective study determined the prevalence of early loss of deciduous molars in patients enrolled at the Pediatric Dentistry clinic at the State University of Paraíba. A review of 515 patient records were analyzed, registered in a form. The following variables were analyzed: gender, age, type of deciduous molar loss, region (maxilla or mandible and side (right and left. It was observed that the prevalence of early tooth loss was 15.1% and there was a similar distribution between the genders. In regard to age, the greatest frequency of tooth loss involved patients at 7 years old (32.1%. There was a similar distribution of tooth loss between the maxilla and mandible regions, at 43.6% each, with the left side being themost involved (41%. The second upper left deciduous molar was the most commonly missing tooth (17.9%, followed by the first upper right deciduous molar (16.1%. It can be concluded that the

  4. The application of coronal scattering measurements to solar radio bursts

    International Nuclear Information System (INIS)

    Bradford, H.M.

    1980-01-01

    The interpretation of ground based observations of solar 'plasma frequency' radio bursts has been hampered in the past by an insufficient knowledge of coronal scattering by density inhomogeneities close to the Sun. Calculations based on measuurements of the angular broadening of natural radio sources, and Woo's 1975 measurement of the angular broadening of the telemetry carrier by Helios I near occultation (Woo, 1978), indicate that plasma frequency solar bursts should undergo considerable scattering, at least near the maximum of the sunspot cycle. The calculated displacements of the apparent positions of the bursts are about equal to the observed displacements which have been attributed to the bursts occurring in dense streamers. In order to obtain more scattering data close to the Sun, interferometer measurements of the angular broadening of spacecraft signals are planned, and the important contribution which could be made with large dishes is discussed. (Auth.)

  5. Latitudinal Dependence of the Radial IMF Component: Coronal Imprint

    Science.gov (United States)

    Suess, S. T.; Smith, E. J.

    1996-01-01

    Measurements by Ulysses have confirmed that there is no significant gradient with respect to heliomagnetic latitude in the radial component, B(sub r,) of the interplanetary magnetic field. In the corona, the plasma, beta is much less than 1, except directly above streamers, so longitudinal and latitudinal gradients in field strength will relax due to the transverse magnetic pressure gradient force as the solar wind carries magnetic flux away from the Sun. This happens quickly enough so that the field is essentially uniform by 5 - 10 solar radius, apparently remaining so as it is carried to beyond 1 AU. Here, we illustrate the coronal relaxation with a qualitative physical argument and by reference to a detailed Magneto HydroDynamics (MHD) simulation.

  6. Changes in the subgingival biofilm composition after coronally positioned flap

    Directory of Open Access Journals (Sweden)

    Jadson Almeida Lima

    2011-02-01

    Full Text Available OBJECTIVES: This study evaluated the effects of coronally positioned flap (CPF on the subgingival biofilm composition. MATERIAL AND METHODS: Twenty-two subjects with gingival recessions were treated with CPF. Clinical parameters were assessed before and at 6 months after surgery. Subgingival biofilms were analyzed by checkerboard DNA-DNA hybridization technique for 40 bacterial species. RESULTS: Recession height, clinical attachment level and bleeding on probing improved significantly (p<0.05 at 6 months post-CPF. The proportions of 10 periodontal pathogens and the proportions of red and orange complexes decreased at 6 months. CONCLUSION: In conclusion, CPF can induce beneficial effects on the composition of the subgingival microbiota after 6 months.

  7. Electron acceleration and radiation signatures in loop coronal transients

    Science.gov (United States)

    Vlahos, L.; Gergely, T. E.; Papadopoulos, K.

    1982-01-01

    It is proposed that in loop coronal transients an erupting loop moves away from the solar surface, with a velocity exceeding the local Alfven speed, pushing against the overlying magnetic fields and driving a shock in the front of the moving part of the loop. Lower hybrid waves are excited at the shock front and propagate radially toward the center of the loop with phase velocity along the magnetic field that exceeds the thermal velocity. The lower hybrid waves stochastically accelerate the tail of the electron distribution inside the loop. The manner in which the accelerated electrons are trapped in the moving loop are discussed, and their radiation signature is estimated. It is suggested that plasma radiation can explain the power observed in stationary and moving type IV bursts.

  8. FAST DIFFERENTIAL EMISSION MEASURE INVERSION OF SOLAR CORONAL DATA

    Energy Technology Data Exchange (ETDEWEB)

    Plowman, Joseph; Kankelborg, Charles; Martens, Petrus [Montana State University, Bozeman, MT 59717 (United States)

    2013-07-01

    We present a fast method for reconstructing differential emission measures (DEMs) using solar coronal data. The method consists of a fast, simple regularized inversion in conjunction with an iteration scheme for removal of residual negative emission measure. On average, it computes over 1000 DEMs s{sup -1} for a sample active region observed by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory, and achieves reduced chi-squared of order unity with no negative emission in all but a few test cases. The high performance of this method is especially relevant in the context of AIA, which images of order one million solar pixels per second. This paper describes the method, analyzes its fidelity, compares its performance and results with other DEM methods, and applies it to an active region and loop observed by AIA and by the Extreme-ultraviolet Imaging Spectrometer on Hinode.

  9. Coronal Polarization of Pseudostreamers and the Solar Polar Field Reversal

    Science.gov (United States)

    Rachmeler, L. A.; Guennou, C.; Seaton, D. B.; Gibson, S. E.; Auchere, F.

    2016-01-01

    The reversal of the solar polar magnetic field is notoriously hard to pin down due to the extreme viewing angle of the pole. In Cycle 24, the southern polar field reversal can be pinpointed with high accuracy due to a large-scale pseudostreamer that formed over the pole and persisted for approximately a year. We tracked the size and shape of this structure with multiple observations and analysis techniques including PROBA2/SWAP EUV images, AIA EUV images, CoMP polarization data, and 3D tomographic reconstructions. We find that the heliospheric field reversed polarity in February 2014, whereas in the photosphere, the last vestiges of the previous polar field polarity remained until March 2015. We present here the evolution of the structure and describe its identification in the Fe XII 1074nm coronal emission line, sensitive to the Hanle effect in the corona.

  10. Solar radio bursts and their relation of coronal magnetic structures

    International Nuclear Information System (INIS)

    Kattenberg, A.

    1981-01-01

    Following a general introduction, chapters II and III describe a model for coronal flux tubes. The model tube is a cylindrically symmetric localized force free current, that is embedded in a potential field. In both chapters the growth rates and sizes of the kink mode instability are calculated by solving the linearized equation of motion. In chapters IV and V, observations of solar Type-I radio bursts are presented and analysed. The observations were gathered with the 60-channel radio spectrograph in Dwingeloo. Chapters VI, VII, VIII, IX and X are concerned with observations of solar microwave bursts. The observations, with high time resolution (0.1 s) and high one-dimensional angular resolution (max. 4'') were made with the Westerbork Synthesis Radio Telescope. (Auth.)

  11. On interplanetary coronal mass ejection identification at 1 AU

    International Nuclear Information System (INIS)

    Mulligan, T.; Russell, C.T.; Gosling, J.T.

    1999-01-01

    Coronal mass ejections are believed to be produced in the corona from closed magnetic regions not previously participating in the solar wind expansion. At 1 AU their interplanetary counterparts (ICMEs) generally have a number of distinct plasma and field signatures that distinguish them from the ambient solar wind. These include heat flux dropouts, bi-directional streaming, enhanced alpha particle events, times of depressed proton temperatures, intervals of distorted or enhanced magnetic field, and times of large magnetic field rotations characteristic of magnetic clouds. The first three of these signatures are phenomena that occur at some point within the ICME, but do not necessarily persist throughout the entire ICME. The large scale magnetic field rotations, distortions and enhancements, and the proton temperature depressions tend to mark more accurately the beginning and end of the ICME proper. We examine herein the reliability with which each of these markers identifies ICMEs utilizing ISEE-3 data from 1978 - 1980. copyright 1999 American Institute of Physics

  12. Shear-induced opening of the coronal magnetic field

    Science.gov (United States)

    Wolfson, Richard

    1995-01-01

    This work describes the evolution of a model solar corona in response to motions of the footpoints of its magnetic field. The mathematics involved is semianalytic, with the only numerical solution being that of an ordinary differential equation. This approach, while lacking the flexibility and physical details of full MHD simulations, allows for very rapid computation along with complete and rigorous exploration of the model's implications. We find that the model coronal field bulges upward, at first slowly and then more dramatically, in response to footpoint displacements. The energy in the field rises monotonically from that of the initial potential state, and the field configuration and energy appraoch asymptotically that of a fully open field. Concurrently, electric currents develop and concentrate into a current sheet as the limiting case of the open field is approached. Examination of the equations shows rigorously that in the asymptotic limit of the fully open field, the current layer becomes a true ideal MHD singularity.

  13. OSO 8 observational limits to the acoustic coronal heating mechanism

    Science.gov (United States)

    Bruner, E. C., Jr.

    1981-01-01

    An improved analysis of time-resolved line profiles of the C IV resonance line at 1548 A has been used to test the acoustic wave hypothesis of solar coronal heating. It is shown that the observed motions and brightness fluctuations are consistent with the existence of acoustic waves. Specific account is taken of the effect of photon statistics on the observed velocities, and a test is devised to determine whether the motions represent propagating or evanescent waves. It is found that on the average about as much energy is carried upward as downward such that the net acoustic flux density is statistically consistent with zero. The statistical uncertainty in this null result is three orders of magnitue lower than the flux level needed to heat the corona.

  14. An ice-cream cone model for coronal mass ejections

    Science.gov (United States)

    Xue, X. H.; Wang, C. B.; Dou, X. K.

    2005-08-01

    In this study, we use an ice-cream cone model to analyze the geometrical and kinematical properties of the coronal mass ejections (CMEs). Assuming that in the early phase CMEs propagate with near-constant speed and angular width, some useful properties of CMEs, namely the radial speed (v), the angular width (α), and the location at the heliosphere, can be obtained considering the geometrical shapes of a CME as an ice-cream cone. This model is improved by (1) using an ice-cream cone to show the near real configuration of a CME, (2) determining the radial speed via fitting the projected speeds calculated from the height-time relation in different azimuthal angles, (3) not only applying to halo CMEs but also applying to nonhalo CMEs.

  15. Exploring the fine structure at the limb in coronal holes

    Science.gov (United States)

    Karovska, Magarita; Blundell, Solon F.; Habbal, Shadia Rifai

    1994-01-01

    The fine structure of the solar limb in coronal holes is explored at temperatures ranging from 10(exp 4) to 10(exp 6) K. An image enhancement algorithm orignally developed for solar eclipse observations is applied to a number of simultaneous multiwavelength observations made with the Harvard Extreme Ultraviolet Spectrometer experiment on Skylab. The enhanced images reveal the presence of filamentary structures above the limb with a characteristic separation of approximately 10 to 15 sec . Some of the structures extend from the solar limb into the corona to at least 4 min above the solar limb. The brightness of these structures changes as a function of height above the limb. The brightest emission is associated with spiculelike structures in the proximity of the limb. The emission characteristic of high-temperature plasma is not cospatial with the emission at lower temperatures, indicating the presence of different temperature plasmas in the field of view.

  16. A NEW VIEW OF CORONAL WAVES FROM STEREO

    International Nuclear Information System (INIS)

    Ma, S.; Lin, J.; Zhao, S.; Li, Q.; Wills-Davey, M. J.; Attrill, G. D. R.; Golub, L.; Chen, P. F.; Chen, H.

    2009-01-01

    On 2007 December 7, there was an eruption from AR 10977, which also hosted a sigmoid. An EUV Imaging Telescope (EIT) wave associated with this eruption was observed by EUVI on board the Solar Terrestrial Relations Observatory (STEREO). Using EUVI images in the 171 A and the 195 A passbands from both STEREO A and B, we study the morphology and kinematics of this EIT wave. In the early stages, images of the EIT wave from the two STEREO spacecrafts differ markedly. We determine that the EUV fronts observed at the very beginning of the eruption likely include some intensity contribution from the associated coronal mass ejection (CME). Additionally, our velocity measurements suggest that the EIT wave front may propagate at nearly constant velocity. Both results offer constraints on current models and understanding of EIT waves.

  17. Einstein Observatory coronal temperatures of late-type stars

    Science.gov (United States)

    Schmitt, J. H. M. M.; Collura, A.; Sciortino, S.; Vaiana, G. S.; Harnden, F. R., Jr.

    1990-01-01

    The results are presented of a survey of the coronal temperatures of late-type stars using the Einstein Observatory IPC. The spectral analysis shows that the frequently found one- and two-temperature descriptions are mainly influenced by the SNR of the data and that models using continuous emission measure distributions can provide equally adequate and physically more meaningful and more plausible descriptions. Intrinsic differences in differential emission measure distributions are found for four groups of stars. M dwarfs generally show evidence for high-temperature gas in conjunction with lower-temperature material, while main-sequence stars of types F and G have the high-temperature component either absent or very weak. Very hot coronae without the lower-temperature component appearing in dwarf stars are evident in most of the giant stars studied. RS CVn systems show evidence for extremely hot coronae, sometimes with no accompanying lower-temperature material.

  18. Transition region, coronal heating and the fast solar wind

    Science.gov (United States)

    Li, Xing

    2003-07-01

    It is assumed that magnetic flux tubes are strongly concentrated at the boundaries of supergranule convection cells. A power law spectrum of high frequency Alfvén waves with a spectral index -1 originating from the sun is assumed to supply all the energy needed to energize the plasma flowing in such magnetic flux tubes. At the high frequency end, the waves are eroded by ions due to ion cyclotron resonance. The magnetic flux concentration is essential since it allows a sufficiently strong energy flux to be carried by high frequency ion cyclotron waves and these waves can be readily released at the coronal base by cyclotron resonance. The main results are: 1. The waves are capable of creating a steep transition region, a hot corona and a fast solar wind if both the wave frequency is high enough and the magnetic flux concentration is sufficiently strong in the boundaries of the supergranule convection zone. 2. By primarily heating alpha particles only, it is possible to produce a steep transition region, a hot corona and a fast solar wind. Coulomb coupling plays a key role in transferring the thermal energy of alpha particles to protons and electrons at the corona base. The electron thermal conduction then does the remaining job to create a sharp transition region. 3. Plasma species (even ions) may already partially lose thermal equilibrium in the transition region, and minor ions may already be faster than protons at the very base of the corona. 4. The model predicts high temperature alpha particles (Talpha ~ 2 x 107 K) and low proton temperatures (Tp solar radii, suggesting that hydrogen Lyman lines observed by UVCS above coronal holes may be primarily broadened by Alfvén waves in this range.

  19. Volumetric measurement of the maxillary sinus by coronal CT scan

    International Nuclear Information System (INIS)

    Ikeda, Atsuko

    1996-01-01

    The volume of the maxillary sinus was estimated by coronal CT scan. The purpose of this study was to compare the estimated volume of the normal maxillary sinus with that of the inflamed maxillary sinus. Patients were classified following evaluation by CT scan of the paranasal sinuses into 3 categories. Group A (n=12): Patients suffered from headache, facial pain and epistaxis, but CT scans of their nasal cavity and paranasal sinus were within normal limits without inflammatory change. Group B (n=69): Patients with bilateral chronic maxillary sinusitis, CT scans of whom showed inflammatory changes in both maxillary sinuses. All of the patients in this group underwent sinus surgery after coronal CT scans. Group C (n=14): Patients with unilateral chronic maxillary sinusitis, CT scans of whom showed inflammatory change in unilateral maxillary sinuses. CT scans of these patients were measured by Plannimeter to take the area of each image of the maxillary sinus. Consecutively imaged areas were summated by integral calculus to obtain an estimate of the sinus volume. The mean maxillary sinus volume in the affected sinuses was significantly smaller than those in the contralateral normal sinuses (p<0.05, Wilcoxon-test). The various volumes of the maxillary sinuses and the developmental cause were discussed. Comparison of groups A with B suggested three distinct patterns; the maxillary sinus volume has decreased due to inflammatory changes in the bone. The small sinuses have a tendency to develop chronic inflammatory change. The aeration in the maxillary sinus may be decreased when anatomic variations that may obstruct the ethmoid infundibulum exist. (K.H.)

  20. Three-Dimensional Morphology of a Coronal Prominence Cavity

    Science.gov (United States)

    Gibson, S. E.; Kucera, T. A.; Rastawicki, D.; Dove, J.; deToma, G.; Hao, J.; Hill, S.; Hudson, H. S.; Marque, C.; McIntosh, P. S.; hide

    2010-01-01

    We present a three-dimensional density model of coronal prominence cavities, and a morphological fit that has been tightly constrained by a uniquely well-observed cavity. Observations were obtained as part of an International Heliophysical Year campaign by instruments from a variety of space- and ground-based observatories, spanning wavelengths from radio to soft-X-ray to integrated white light. From these data it is clear that the prominence cavity is the limb manifestation of a longitudinally-extended polar-crown filament channel, and that the cavity is a region of low density relative to the surrounding corona. As a first step towards quantifying density and temperature from campaign spectroscopic data, we establish the three-dimensional morphology of the cavity. This is critical for taking line-of-sight projection effects into account, since cavities are not localized in the plane of the sky and the corona is optically thin. We have augmented a global coronal streamer model to include a tunnel-like cavity with elliptical cross-section and a Gaussian variation of height along the tunnel length. We have developed a semi-automated routine that fits ellipses to cross-sections of the cavity as it rotates past the solar limb, and have applied it to Extreme Ultraviolet Imager (EUVI) observations from the two Solar Terrestrial Relations Observatory (STEREO) spacecraft. This defines the morphological parameters of our model, from which we reproduce forward-modeled cavity observables. We find that cavity morphology and orientation, in combination with the viewpoints of the observing spacecraft, explains the observed variation in cavity visibility for the east vs. west limbs

  1. THE CORONAL LOOP INVENTORY PROJECT: EXPANDED ANALYSIS AND RESULTS

    Energy Technology Data Exchange (ETDEWEB)

    Schmelz, J. T. [USRA, 7178 Columbia Gateway Drive, Columbia, MD 21046 (United States); Christian, G. M.; Chastain, R. A., E-mail: jschmelz@usra.edu [Physics Department, University of Memphis, Memphis, TN 38152 (United States)

    2016-11-10

    We have expanded upon earlier work that investigates the relative importance of coronal loops with isothermal versus multithermal cross-field temperature distributions. These results are important for determining if loops have substructure in the form of unresolved magnetic strands. We have increased the number of loops targeted for temperature analysis from 19 to 207 with the addition of 188 new loops from multiple regions. We selected all loop segments visible in the 171 Å images of the Atmospheric Imaging Assembly (AIA) that had a clean background. Eighty-six of the new loops were rejected because they could not be reliably separated from the background in other AIA filters. Sixty-one loops required multithermal models to reproduce the observations. Twenty-eight loops were effectively isothermal, that is, the plasma emission to which AIA is sensitive could not be distinguished from isothermal emission, within uncertainties. Ten loops were isothermal. Also, part of our inventory was one small flaring loop, one very cool loop whose temperature distribution could not be constrained by the AIA data, and one loop with inconclusive results. Our survey can confirm an unexpected result from the pilot study: we found no isothermal loop segments where we could properly use the 171-to-193 ratio method, which would be similar to the analysis done for many loops observed with TRACE and EIT. We recommend caution to observers who assume the loop plasma is isothermal, and hope that these results will influence the direction of coronal heating models and the effort modelers spend on various heating scenarios.

  2. Volumetric measurement of the maxillary sinus by coronal CT scan

    Energy Technology Data Exchange (ETDEWEB)

    Ikeda, Atsuko [Tokyo Medical and Dental Univ. (Japan). School of Medicine

    1996-08-01

    The volume of the maxillary sinus was estimated by coronal CT scan. The purpose of this study was to compare the estimated volume of the normal maxillary sinus with that of the inflamed maxillary sinus. Patients were classified following evaluation by CT scan of the paranasal sinuses into 3 categories. Group A (n=12): Patients suffered from headache, facial pain and epistaxis, but CT scans of their nasal cavity and paranasal sinus were within normal limits without inflammatory change. Group B (n=69): Patients with bilateral chronic maxillary sinusitis, CT scans of whom showed inflammatory changes in both maxillary sinuses. All of the patients in this group underwent sinus surgery after coronal CT scans. Group C (n=14): Patients with unilateral chronic maxillary sinusitis, CT scans of whom showed inflammatory change in unilateral maxillary sinuses. CT scans of these patients were measured by Plannimeter to take the area of each image of the maxillary sinus. Consecutively imaged areas were summated by integral calculus to obtain an estimate of the sinus volume. The mean maxillary sinus volume in the affected sinuses was significantly smaller than those in the contralateral normal sinuses (p<0.05, Wilcoxon-test). The various volumes of the maxillary sinuses and the developmental cause were discussed. Comparison of groups A with B suggested three distinct patterns; the maxillary sinus volume has decreased due to inflammatory changes in the bone. The small sinuses have a tendency to develop chronic inflammatory change. The aeration in the maxillary sinus may be decreased when anatomic variations that may obstruct the ethmoid infundibulum exist. (K.H.)

  3. Perdurabilidad empresarial: concepto, estudios, hallazgos

    Directory of Open Access Journals (Sweden)

    Hugo Alberto Rivera Rodríguez

    2012-06-01

    Full Text Available La literatura en dirección de empresas durante los últimos 20 años ha analizado diferentes aspectos de la perdurabilidad empresarial, sobre todo lo relacionado con el papel del líder, la asociación con la rentabilidad, y los efectos que genera en el tejido empresarial. Sin embargo, aún existen muchos aspectos en los cuales se debe profundizar. El primero de ellos es dar solución a la diversidad terminológica existente. Al no tener un consenso sobre el concepto, se utilizan de manera indiscriminada términos como longevidad, sostenibilidad, éxito, supervivencia, duración, etc., los cuales en lugar de aclarar, generan confusión. Por otro lado, tampoco hay evidencia suficiente para sugerir alternativas que permitan a las empresas lograr ser perdurables. El artículo que se presenta se fundamenta en una revisión exhaustiva del concepto de perdurabilidad empresarial, y hace una relación de los principales hallazgos encontrados en la literatura sobre las condiciones que pueden facilitar la perdurabilidad empresarial. Con ello se pretende de avanzar en el estudio de la relación entre la perdurabilidad, el comportamiento estratégico de las empresas y desempeño financiero.

  4. Assessment of T2-Weighted Coronal Magnetic Resonance Images in the Investigation of Pituitary Lesions

    International Nuclear Information System (INIS)

    Yuksekkaya, Ruken; Aggunlu, Levent; Oner, Yusuf; Celik, Halil; Akpek, Sergin; Celikyay, Fatih

    2014-01-01

    Magnetic resonance imaging is the most important diagnostic method in the investigation of the pituitary lesions. Our aim is to determine whether T2-weighted coronal images may be helpful in the evaluation of the pituitary gland with suspected pituitary adenomas. One hundred and sixty-seven patients were examined prospectively with T2-weighted coronal and T1-weighted coronal images enhanced with intravenous contrast material. The images were evaluated for the presence, the size, the location, and the ancillary signs including sellar floor erosion or ballooning, infindibulary deviation, convexity of the superior border of the gland, diffuse enlargement of the gland, and the invasion of the cavenous sinuses on both images. In forty-six (28%) patients lesions were revealed on both sequences. In twenty-one (12%) patients the lesions that were revealed on the T1-weighted images were not detected on the T2-weighted images. Positive predictive value, negative predictive value, sensitivity, specificity, and diagnostic accuracy rates of T2-weighted coronal images on the detection of the presence of lesions were 100%, 17.4%, 68.7%, 100%, and 87.4%, respectively. Both T2-weighted coronal and T1-weighted coronal images enhanced with intravenous gadolinium-based contrast material are important in the diagnosis of pituitary adenomas. T2-weighted coronal images could be used as a screening tool for the primary evaluation of the pituitary gland

  5. 3D Global Coronal Density Structure and Associated Magnetic Field near Solar Maximum

    Energy Technology Data Exchange (ETDEWEB)

    Kramar, Maxim [Physics Department, The Catholic University of America, Washington, DC (United States); Airapetian, Vladimir [Department of Physics and Astronomy, George Mason University, Fairfax, VA (United States); NASA/Goddard Space Flight Center, Code 671, Greenbelt, MD (United States); Lin, Haosheng, E-mail: vladimir.airapetian@nasa.gov [College of Natural Sciences, Institute for Astronomy, University of Hawaii at Manoa, Pukalani, HI (United States)

    2016-08-09

    Measurement of the coronal magnetic field is a crucial ingredient in understanding the nature of solar coronal dynamic phenomena at all scales. We employ STEREO/COR1 data obtained near maximum of solar activity in December 2012 (Carrington rotation, CR 2131) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from 1.5 to 4 R{sub ⊙} using a tomography method and qualitatively deduce structures of the coronal magnetic field. The 3D electron density analysis is complemented by the 3D STEREO/EUVI emissivity in 195 Å band obtained by tomography for the same CR period. We find that the magnetic field configuration during CR 2131 has a tendency to become radially open at heliocentric distances below ~2.5 R{sub ⊙}. We compared the reconstructed 3D coronal structures over the CR near the solar maximum to the one at deep solar minimum. Results of our 3D density reconstruction will help to constrain solar coronal field models and test the accuracy of the magnetic field approximations for coronal modeling.

  6. Observations and Numerical Models of Solar Coronal Heating Associated with Spicules

    Energy Technology Data Exchange (ETDEWEB)

    Pontieu, B. De; Martinez-Sykora, J. [Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Org. A021S, Building 252, Palo Alto, CA 94304 (United States); Moortel, I. De [School of Mathematics and Statistics, University of St Andrews, St Andrews, Fife KY16 9SS (United Kingdom); McIntosh, S. W. [High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307 (United States)

    2017-08-20

    Spicules have been proposed as significant contributors to the mass and energy balance of the corona. While previous observations have provided a glimpse of short-lived transient brightenings in the corona that are associated with spicules, these observations have been contested and are the subject of a vigorous debate both on the modeling and the observational side. Therefore, it remains unclear whether plasma is heated to coronal temperatures in association with spicules. We use high-resolution observations of the chromosphere and transition region (TR) with the Interface Region Imaging Spectrograph and of the corona with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to show evidence of the formation of coronal structures associated with spicular mass ejections and heating of plasma to TR and coronal temperatures. Our observations suggest that a significant fraction of the highly dynamic loop fan environment associated with plage regions may be the result of the formation of such new coronal strands, a process that previously had been interpreted as the propagation of transient propagating coronal disturbances. Our observations are supported by 2.5D radiative MHD simulations that show heating to coronal temperatures in association with spicules. Our results suggest that heating and strong flows play an important role in maintaining the substructure of loop fans, in addition to the waves that permeate this low coronal environment.

  7. 3D Global Coronal Density Structure and Associated Magnetic Field near Solar Maximum

    Directory of Open Access Journals (Sweden)

    Maxim Kramar

    2016-08-01

    Full Text Available Measurement of the coronal magnetic field is a crucial ingredient in understanding the nature of solar coronal dynamic phenomena at all scales. We employ STEREO/COR1 data obtained near maximum of solar activity in December 2012 (Carrington rotation, CR 2131 to retrieve and analyze the three-dimensional (3D coronal electron density in the range of heights from $1.5$ to $4 R_odot$ using a tomography method and qualitatively deduce structures of the coronal magnetic field. The 3D electron density analysis is complemented by the 3D STEREO/EUVI emissivity in 195 AA band obtained by tomography for the same CR period. We find that the magnetic field configuration during CR 2131 has a tendency to become radially open at heliocentric distances below $sim 2.5 R_odot$. We compared the reconstructed 3D coronal structures over the CR near the solar maximum to the one at deep solar minimum. Results of our 3D density reconstruction will help to constrain solar coronal field models and test the accuracy of the magnetic field approximations for coronal modeling.

  8. VECTOR TOMOGRAPHY FOR THE CORONAL MAGNETIC FIELD. II. HANLE EFFECT MEASUREMENTS

    International Nuclear Information System (INIS)

    Kramar, M.; Inhester, B.; Lin, H.; Davila, J.

    2013-01-01

    In this paper, we investigate the feasibility of saturated coronal Hanle effect vector tomography or the application of vector tomographic inversion techniques to reconstruct the three-dimensional magnetic field configuration of the solar corona using linear polarization measurements of coronal emission lines. We applied Hanle effect vector tomographic inversion to artificial data produced from analytical coronal magnetic field models with equatorial and meridional currents and global coronal magnetic field models constructed by extrapolation of real photospheric magnetic field measurements. We tested tomographic inversion with only Stokes Q, U, electron density, and temperature inputs to simulate observations over large limb distances where the Stokes I parameters are difficult to obtain with ground-based coronagraphs. We synthesized the coronal linear polarization maps by inputting realistic noise appropriate for ground-based observations over a period of two weeks into the inversion algorithm. We found that our Hanle effect vector tomographic inversion can partially recover the coronal field with a poloidal field configuration, but that it is insensitive to a corona with a toroidal field. This result demonstrates that Hanle effect vector tomography is an effective tool for studying the solar corona and that it is complementary to Zeeman effect vector tomography for the reconstruction of the coronal magnetic field

  9. Recurring coronal holes and their rotation rates during the solar cycles 22-24

    Science.gov (United States)

    Prabhu, K.; Ravindra, B.; Hegde, Manjunath; Doddamani, Vijayakumar H.

    2018-05-01

    Coronal holes (CHs) play a significant role in making the Earth geo-magnetically active during the declining and minimum phases of the solar cycle. In this study, we analysed the evolutionary characteristics of the Recurring CHs from the year 1992 to 2016. The extended minimum of Solar Cycle 23 shows unusual characteristics in the number of persistent coronal holes in the mid- and low-latitude regions of the Sun. Carrington rotation maps of He 10830 Å and EUV 195 Å observations are used to identify the Coronal holes. The latitude distribution of the RCHs shows that most of them are appeared between ± 20° latitudes. In this period, more number of recurring coronal holes appeared in and around 100° and 200° Carrington longitudes. The large sized coronal holes lived for shorter period and they appeared close to the equator. From the area distribution over the latitude considered, it shows that more number of recurring coronal holes with area <10^{21} cm2 appeared in the southern latitude close to the equator. The rotation rates calculated from the RCHs appeared between ± 60° latitude shows rigid body characteristics. The derived rotational profiles of the coronal holes show that they have anchored to a depth well below the tachocline of the interior, and compares well with the helioseismology results.

  10. Relationship between coronal holes and high speed streams at L1: arrival times, durations, and intensities

    Science.gov (United States)

    Luo, B.; Bu, X.; Liu, S.; Gong, J.

    2017-12-01

    Coronal holes are sources of high-speed steams (HSS) of solar wind. When coronal holes appear at mid/low latitudes on the Sun, consequential HSSs may impact Earth and cause recurrent geospace environment disturbances, such as geomagnetic storms, relativistic electron enhancements at the geosynchronous orbit, and thermosphere density enhancements. Thus, it is of interests for space weather forecasters to predict when (arrival times), how long (time durations), and how severe (intensities) HSSs may impact Earth when they notice coronal holes on the sun and are anticipating their geoeffectiveness. In this study, relationship between coronal holes and high speed streams will be statistically investigated. Several coronal hole parameters, including passage times of solar central meridian, coronal hole longitudinal widths, intensities reflected by mean brightness, are derived using Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) images for years 2011 to 2016. These parameters will be correlated with in-situ solar wind measurements measured at the L1 point by the ACE spacecraft, which can give some results that are useful for space weather forecaster in predicting the arrival times, durations, and intensities of coronal hole high-speed streams in about 3 days advance.

  11. Two-zone model of coronal hole structure in the high corona

    International Nuclear Information System (INIS)

    Wang, Z.; Kundu, M.R.; Yoshimura, H.

    1988-01-01

    The two-zone coronal hole structure model presently proposed for the high corona at 1.5-1.7 solar radii emerges from a comparison of computation results for the potential magnetic fields of the corona and meter-decameter radio observations. The two zones of a coronal hole are defined by the configuration of magnetic field lines around a coronal hole: (1) the central hole of an open diverging magnetic field line system; and (2) the boundary zone between the central zone of the open field line system and the closed field line system or systems surrounding the open field line system. 19 references

  12. Non-adversarial justice and the coroner's court: a proposed therapeutic, restorative, problem-solving model.

    Science.gov (United States)

    King, Michael S

    2008-12-01

    Increasingly courts are using new approaches that promote a more comprehensive resolution of legal problems, minimise any negative effects that legal processes have on participant wellbeing and/or that use legal processes to promote participant wellbeing. Therapeutic jurisprudence, restorative justice, mediation and problem-solving courts are examples. This article suggests a model for the use of these processes in the coroner's court to minimise negative effects of coroner's court processes on the bereaved and to promote a more comprehensive resolution of matters at issue, including the determination of the cause of death and the public health and safety promotion role of the coroner.

  13. CORONAL MAGNETIC FIELDS DERIVED FROM SIMULTANEOUS MICROWAVE AND EUV OBSERVATIONS AND COMPARISON WITH THE POTENTIAL FIELD MODEL

    Energy Technology Data Exchange (ETDEWEB)

    Miyawaki, Shun; Nozawa, Satoshi [Department of Science, Ibaraki University, Mito, Ibaraki 310-8512 (Japan); Iwai, Kazumasa; Shibasaki, Kiyoto [Nobeyama Solar Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Nagano 384-1305 (Japan); Shiota, Daikou, E-mail: shunmi089@gmail.com [Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8601 (Japan)

    2016-02-10

    We estimated the accuracy of coronal magnetic fields derived from radio observations by comparing them to potential field calculations and the differential emission measure measurements using EUV observations. We derived line-of-sight components of the coronal magnetic field from polarization observations of the thermal bremsstrahlung in the NOAA active region 11150, observed around 3:00 UT on 2011 February 3 using the Nobeyama Radioheliograph at 17 GHz. Because the thermal bremsstrahlung intensity at 17 GHz includes both chromospheric and coronal components, we extracted only the coronal component by measuring the coronal emission measure in EUV observations. In addition, we derived only the radio polarization component of the corona by selecting the region of coronal loops and weak magnetic field strength in the chromosphere along the line of sight. The upper limits of the coronal longitudinal magnetic fields were determined as 100–210 G. We also calculated the coronal longitudinal magnetic fields from the potential field extrapolation using the photospheric magnetic field obtained from the Helioseismic and Magnetic Imager. However, the calculated potential fields were certainly smaller than the observed coronal longitudinal magnetic field. This discrepancy between the potential and the observed magnetic field strengths can be explained consistently by two reasons: (1) the underestimation of the coronal emission measure resulting from the limitation of the temperature range of the EUV observations, and (2) the underestimation of the coronal magnetic field resulting from the potential field assumption.

  14. Funciones profesorales: un estudio factorial

    Directory of Open Access Journals (Sweden)

    Pedro S. de VICENTE RODRÍGUEZ

    2009-11-01

    Full Text Available La preocupación por la «cantidad» ha privado durante mucho tiempo en el ámbito educativo; ha sido considerado esencial por los gobiernos la consecución de una «educación para todos». Sin embargo, el aumento de los costos no ha conllevado una mejora sustancial, una disminución efectiva de la ineficacia de los sistemas tradicionales de enseñanza; de ello dan fe las tasas de abandonos y repeticiones de curso. Esto conduce a considerar que la falta de correspondencia entre el aumento de los recursos destinados a educación y el rendimiento de las instituciones educativas sea un problema de «calidad» más que de «cantidad». De ahí que se hable hoy insistentemente de la mejora de la calidad de la educación. Al tema de la «calidad de la educación» se dedicó en 1981 un seminario organizado por la Escuela Asturiana de estudios Hispánicos. En él, Víctor García Hoz definía la calidad educativa «como el modo de ser de la educación que reúne las características de integridad, coherencia y eficacia»1, entendiendo la eficacia como la denotación de que el fin perseguido ha sido alcanzado, más que como producción de algo material, con lo que es posible hablar en términos de eficacia refiriéndose tanto a lo cuantitativo como a lo cualitativo.

  15. Artrodese do quadril: estudo retrospectivo com mais de 20 anos de seguimento Hip arthrodesis: a minimum 20 year follow-up retrospective study

    Directory of Open Access Journals (Sweden)

    José Ricardo Negreiros Vicente

    2011-01-01

    Full Text Available OBJETIVO: Avaliar os resultados a longo prazo de setenta pacientes submetidos à artrodese do quadril pela técnica original descrita por Davis. MÉTODOS: Realizamos um estudo clínico retrospectivo com 70 pacientes, operados entre 1982 e 1995. A presença de sintomas sobre a coluna lombar, joelho ipsilateral e quadril contralateral foi aferida assim como o sucesso da consolidação da artrodese, o posicionamento da mesma e a eventual indicação para conversão à artroplastia total do quadril. RESULTADOS: O tempo médio de seguimento foi 21,6 anos. Uma consolidação satisfatória foi constatada em 48 pacientes (85,7%. A dor lombar foi presente em 11 pacientes (19,6% e osteoartrite dolorosa do joelho em quatro pacientes (7,1%. Discussão: Dois trabalhos com seguimento superior ao nosso estudo ( 35 e 38 anos apresentaram repercussões sobre a coluna lombar mais prevalentes (57% e 62%, assim como dor no joelho homolateral (45% e 57% e indicação para conversão em artroplastia total do quadril (17% e 28%. CONCLUSÃO: Concluímos que a artrodese do quadril pela técnica de Davis apresenta resultados satisfatórios até o vigésimo ano, porém a presença de dor lombar é mais frequente com o passar dos anos e a dor no joelho homolateral sugere associação com a posição inicial em abdução do quadril artrodesado. Nivel de Evidência III, estudo clinico.OBJECTIVE: To evaluate the long-term results of seventy patients who underwent hip arthrodesis using the original technique described by Davis. METHODS: We carried out a retrospective study involving seventy patients submitted to hip arthrodesis between 1982 and 1995. The presence of symptoms involving the lumbar spine, ipsilateral knee, and contralateral hip was noted, as well as the success of the arthrodesis fusion, its positioning, and the need for conversion surgery to total hip replacement. RESULTS: The mean follow-up time was 21.6 years. A satisfactory hip fusion was found in 48 patients

  16. Facial fractures: a 1-year retrospective study in a hospital in Belo Horizonte Fraturas de face: um estudo retrospectivo de 1 ano em um hospital de Belo Horizonte

    Directory of Open Access Journals (Sweden)

    Bruno Ramos Chrcanovic

    2004-12-01

    Full Text Available A retrospective study was performed to assess facial fractures in patients treated at a public hospital in Belo Horizonte, in 2000. The data collected included age, gender, etiology, distribution of maxillofacial trauma considering day of the week and month, anatomic site of the fracture, and treatment. The analyses involved descriptive statistics and chi-squared test, Bonferroni test and analysis of variance. A total of 1,326 facial fractures were found in 911 patients. Most fractures occurred in adults with age ranging from 21 to 30 years. Men were more affected than women, with a male-female ratio of 4.69:1. Accidents causing facial fractures occurred predominantly on weekends. Bicycle and motorcycle accidents were the major cause of trauma, followed by interpersonal violence, automobile accidents, and falls. When the relation between the gender and the etiology of facial fractures was analyzed, a significant relation was noted between these variables (p Um estudo retrospectivo foi realizado para avaliar fraturas faciais em pacientes atendidos no ano de 2000 em um hospital público de Belo Horizonte. As informações coletadas incluíam idade, sexo, etiologia, distribuição do trauma de acordo com o dia da semana e o mês, o local anatômico da fratura e o tratamento. As análises envolveram estatísticas descritivas, teste qui-quadrado, teste Bonferroni e análise de variância. Foram encontradas 1.326 fraturas de face em 911 pacientes. A maioria das fraturas ocorreu em adultos na faixa etária de 21 a 30 anos. Os homens foram mais acometidos do que as mulheres, numa proporção homem:mulher de 4,69:1. Os traumas causadores de fraturas faciais ocorreram predominantemente nos fins de semana. Os acidentes de moto e bicicleta foram a maior causa de trauma, seguidos por violência interpessoal, acidentes automobilísticos e quedas. Quando analisada a relação entre o gênero e a etiologia das fraturas de face, observou-se uma associa

  17. Elevação da lipase e amilase no doente crítico: estudo retrospectivo Increased lipase and amilase levels in critically ill patients: retrospective study

    Directory of Open Access Journals (Sweden)

    Margarida Ferreira

    2008-12-01

    Full Text Available OBJETIVOS: A elevação da lipase e amilase séricas são frequentemente encontradas em doentes internados em unidade de terapia intensiva sem que exista doença pancreática prévia, constituindo um desafio diagnóstico e terapêutico. Baseados nesta evidência os autores propuseram-se a determinar a incidência de hiperlipasemia assintomática nos doentes críticos, fatores desencadeantes e evolução clínica destes doentes. MÉTODOS: Estudo retrospectivo dos doentes internados na unidade de terapia intensiva de 1 de janeiro a 31 de dezembro de 2006, excluídas internações por pancreatite aguda, história de patologia pancreática, insuficiência renal ou falta de dados. Pacientes foram distribuídos em dois grupos (com e sem hiperlipasemia e feita comparação considerando diversas variáveis clínicas, laboratoriais, imagiológicas. Análise estatística: SPSS 13; testes t de Student e qui² (IC 95%, com significância estatística se p38 ºC (pOBJECTIVES: Elevated lipase and amylase are commonly found in patients in intensive care unit without a previously recognized pancreatic illness, constituting a diagnostic and therapeutic challenge. The authors therefore proposed to determine the frequency of asymptomatic high serum lipase in critically ill patients, involved risk factors and outcome. METHODS: Retrospective study of patients admitted in an intensive care unit from January 1 to December 31, 2006, excluding admissions for acute pancreatitis, history of pancreatic disease, renal insufficiency or lacking of data. Patients were divided in two groups (with and without high serum lipase that were compared for clinical, laboratory and radiological variables. Statistical analysis: SPSS 13; Student's t test and Chi-square test (CI 95% with statistical significance if p< 0.05. RESULTS: 102 patients were included with high serum lipase was present in 39.2% of patients, mean lipase of 797U/L. Patients with high serum lipase had longer hospital

  18. Clinical etiology of myiasis in ENT: a reterograde period - interval study Etiologia clínica da miíase em otorrinolaringologia: um estudo retrospectivo

    Directory of Open Access Journals (Sweden)

    Shitij Arora

    2009-06-01

    Full Text Available Myiasis in ENT, once a deadly disease still presents as a significant outdoor problem, though advances in management including supportive therapy has led to early healing with significant reduction in bed occupancy rate. AIMS: To assess the clinico etiology, relationship of myiasis to habit and habitat of patients and to assess the changes in age, seasonal, socioeconomic incidence, nasal bacterial flora and usefulness of certain commonly done tests with reference to a gap of 25 years. MATERIALS & METHODS: The presenting study was conducted on 80 patients selected over a period of two time intervals ; first 40 cases were chosen from 1979 to 1980 and next 40 over 2003 to 2004. Cases were studied in a retrograde manner and data tabulated. RESULTS & CONCLUSIONS: Atrophic turbinates was the commonest pathological finding in nose in 30% of cases . Significant change seen was in the age group 51 and above with a rise of 30%. Mode during 2003-04 was 60 years. Incidence of palatal perforation dropped from 17.88 to 2.5% . Klebsiella emerged as a significant contributor to the nasal microbial flora. VDRL and split skin smear showed poor etiological association for the diseases.Miíase em ORL não é mais uma doença fatal, mas ainda está presente como um significativo problema em ambientes externos. Entretanto, progressos alcançados no tratamento, incluindo terapêutica de suporte, têm levado à cura precoce com significativa redução na taxa de internação hospitalar por causa dessa enfermidade. OBJETIVOS: Avaliar a etiologia clínica e as associações entre miíase e os hábitos e habitats dos pacientes; e avaliar diferenças no tocante à idade, estação do ano, incidência socioeconômica, flora bacteriana nasal e a utilidade de certos exames comumente feitos - um estudo retrospectivo de 25 anos. MATERIAIS E MÉTODOS: O presente estudo envolveu 80 pacientes selecionados em dois períodos; os primeiros 40 casos foram selecionados de 1979 a 1980

  19. Retrospective study (1998-2001 on canine ehrlichiosis in Belo Horizonte, MG, Brazil Estudo retrospectivo (1998 a 2001 da erliquiose canina em Belo Horizonte

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    S.M. Moreira

    2003-04-01

    Full Text Available The present work describes a retrospective study of clinical cases of ehrlichiosis in dogs examined from March 1998 to September 2001. From the clinical records with laboratorial confirmation of Ehrlichia canis or E. platys infections, the following parameters were analyzed: demographic aspects (age, race, sex, period of the year and origin, clinical characteristics (body temperature, exposure to ticks and clinical signs, and hematological characteristics (blood cell counts and type of infected cell. A total of 194 clinical records were analyzed, from which 31 animals were infected with E. canis and 21 animals with E. platys. The number of cases of canine ehrlichiosis increased considerably from the year 2000 onwards, and 24.4% of the cases occurred in 13- to 24-month-old animals, in different urban and per-urban regions of the municipality of Belo Horizonte. The most frequent symptoms were fever, anorexia, apathy, abdominal pain, lymphadenopathy and dispnea. Regarding hematological alterations, 70.3% of the animals presented anemia, 50% presented thrombocytopenia and 30% leukopenia, and most E. canis morulae were seen in monocytes. The results point to the importance of canine ehrlichiosis, as 35.9% of the dogs with suspected hemoparasitic diseases were infected with Ehrlichia canis or E. platys.O presente trabalho descreve um estudo retrospectivo da casuística clínica de erliquiose em cães atendidos entre março de 1998 e setembro de 2001. Foram analisadas 194 fichas clínicas de animais com suspeita de hemoparasitoses, nas quais 31 cães foram diagnosticados com Ehrlichia canis e 21 com Ehrlichia platys, por meio de exame parasitológico direto de esfregaços sangüíneos. Foram considerados alguns aspectos demográficos (idade, raça, sexo, época do ano e região de origem, características clínicas (temperatura corporal, presença e/ou histórico de carrapatos e sinais clínicos e hematológicas (hemograma completo e célula parasitada

  20. Estudio farmacoepidemiológico de uso de antiinflamatorios no esteroideos en pacientes de alto riesgo cardiovascular

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    Jorge Enrique Machado-Alba

    Full Text Available Con el objetivo de determinar la frecuencia de uso prolongado de antiinflamatorios no esteroideos (AINES en pacientes colombianos de alto riesgo cardiovascular (ARC se desarrolló un estudio retrospectivo en el cual se identificaron pacientes de ARC que usaron AINES por más de cinco meses continuos entre enero de 2011 y marzo de 2013. Se identificó a los pacientes que recibían crónicamente nitratos, digitálicos, y clopidogrel y ácido acetil salicílico (ASA, quienes fueron identificados como de ARC. Se realizó un análisis de frecuencias de uso según la comedicación recibida. Se encontró uso concomitante de AINES en el 0,35% de los consumidores de nitratos (tiempo promedio: 9,5 ± 4,4 meses, en el 0,36% de los consumidores de clopidogrel y ASA (tiempo promedio: 9,3 ± 3,4 meses, y en el 0,4% de los consumidores de digitálicos (10,2 ± 4,6 meses. Se concluye que existe una baja proporción de uso de AINES de manera crónica en pacientes de alto riesgo cardiovascular.

  1. Comportamiento de la cirugía mayor ambulatoria: Estudio de 5 años

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    Gilberto Martínez Ramos

    2003-12-01

    Full Text Available Se realizó un estudio descriptivo, longitudinal y retrospectivo de 2 208 pacientes operados por el método de cirugía mayor ambulatoria en el servicio de cirugía del Hospital Militar Clinicoquirúrgico Docente "Comandante Manuel Fajardo Rivero" de Santa Clara, durante el período comprendido desde enero de 1997 hasta diciembre del 2001, con el propósito de demostrar las ventajas de este método para el paciente y para la institución. Los pacientes operados de hernias inguinales, epigástricas y umbilicales fueron los que predominaron. También fueron tratados por este método pacientes con litiasis vesicular, fibromiomas uterinos, nódulos de mamas, ginecomastias y hemorroides. Del total de los pacientes la mayor cantidad pertenecía al sexo femenino y en cuanto a la edad los grupos comprendidos entre 20 y 49 años fueron los que más se beneficiaron con este método. Los tipos de anestesia con preferencia a ser utilizados en estos pacientes fueron la anestesia regional y la analgesia quirúrgica acupunturalA descriptive, cross-sectional and prospective study was conducted among 2 208 patients operated on by ambulatory major surgery at the surgery service of "Comandante Manuel Fajardo Rivero" Military Clinical and Surgical Hospital, in Santa Clara, from January, 1997, to December, 2001, aimed at showing the advantages of this method for the patient and the health institution. The patients operated on of inguinal, epigastric and umbilical hernias predominated. This method was also used with vesicular lithiasis, uterine fibromyomas, breast nodules, gynecomasties and hemorrhoids. Most of the patients were females and the groups aged 20-49 were the most benefitted with this method. The types of anesthesia preferably used were regional anesthesia and acupunctural surgical analgesia

  2. Trans trochanteric approach with coronal osteotomy of the great trochanter

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    Steffann Francois

    2015-01-01

    Full Text Available Several surgical approaches could be used in hip arthroplasty or trauma surgery: anterior, anterolateral, lateral, posterior (with or without trochanterotomy, using or not an orthopedic reduction table. Subtrochanteric and extra-capsular trochanteric fractures (ECTF are usually treated by internal fixation with mandatory restrictions on weight bearing. Specific complications have been widely described. Mechanical failures are particularly high in unstable fractures. Hip fractures are a major public health issue with a mortality rate of 12%–23% at 1 year. An alternative option is to treat ECTF by total hip arthroplasty (THA to prevent decubitus complications, to help rapid recovery, and to permit immediate weight bearing as well as quick rehabilitation. However, specific risks of THA have to be considered such as dislocation or cardiovascular failure. The classical approach (anterior or posterior requires the opening of the joint and capsule, weakening hip stability and the repair of the great trochanter is sometimes hazardous. For 15 years, we have been treating unstable ECTF by THA with cementless stem, dual mobility cup (DMC, greater trochanter (GT reattachment, and a new surgical approach preserving capsule, going through the fracture and avoiding joint dislocation. Bombaci first described a similar approach in 2008; our trans fractural digastric approach (medial gluteus and lateral vastus is different. A coronal GT osteotomy is performed when there is no coronal fracture line. It allows easy access to the femoral neck and acetabulum. The THA is implanted without femoral internal rotation to avoid extra bone fragment displacement. With pre-operative planning, cup implantation is easy and stem positioning is adjusted referring to the top of the GT after trial reduction and preoperative planning. The longitudinal osteotomy and trochanteric fracture are repaired with wires and the digastric incision is closed. This variant of Bombaci

  3. Fitting and Reconstruction of Thirteen Simple Coronal Mass Ejections

    Science.gov (United States)

    Al-Haddad, Nada; Nieves-Chinchilla, Teresa; Savani, Neel P.; Lugaz, Noé; Roussev, Ilia I.

    2018-05-01

    Coronal mass ejections (CMEs) are the main drivers of geomagnetic disturbances, but the effects of their interaction with Earth's magnetic field depend on their magnetic configuration and orientation. Fitting and reconstruction techniques have been developed to determine important geometrical and physical CME properties, such as the orientation of the CME axis, the CME size, and its magnetic flux. In many instances, there is disagreement between different methods but also between fitting from in situ measurements and reconstruction based on remote imaging. This could be due to the geometrical or physical assumptions of the models, but also to the fact that the magnetic field inside CMEs is only measured at one point in space as the CME passes over a spacecraft. In this article we compare three methods that are based on different assumptions for measurements by the Wind spacecraft for 13 CMEs from 1997 to 2015. These CMEs are selected from the interplanetary coronal mass ejections catalog on https://wind.nasa.gov/ICMEindex.php https://wind.nasa.gov/ICMEindex.php" TargetType="URL"/> because of their simplicity in terms of: 1) slow expansion speed throughout the CME and 2) weak asymmetry in the magnetic field profile. This makes these 13 events ideal candidates for comparing codes that do not include expansion or distortion. We find that for these simple events, the codes are in relatively good agreement in terms of the CME axis orientation for six of the 13 events. Using the Grad-Shafranov technique, we can determine the shape of the cross-section, which is assumed to be circular for the other two models, a force-free fitting and a circular-cylindrical non force-free fitting. Five of the events are found to have a clear circular cross-section, even when this is not a precondition of the reconstruction. We make an initial attempt at evaluating the adequacy of the different assumptions for these simple CMEs. The conclusion of this work strongly suggests that attempts

  4. Identification of coronal heating events in 3D simulations

    Science.gov (United States)

    Kanella, Charalambos; Gudiksen, Boris V.

    2017-07-01

    Context. The solar coronal heating problem has been an open question in the science community since 1939. One of the proposed models for the transport and release of mechanical energy generated in the sub-photospheric layers and photosphere is the magnetic reconnection model that incorporates Ohmic heating, which releases a part of the energy stored in the magnetic field. In this model many unresolved flaring events occur in the solar corona, releasing enough energy to heat the corona. Aims: The problem with the verification and quantification of this model is that we cannot resolve small scale events due to limitations of the current observational instrumentation. Flaring events have scaling behavior extending from large X-class flares down to the so far unobserved nanoflares. Histograms of observable characteristics of flares show powerlaw behavior for energy release rate, size, and total energy. Depending on the powerlaw index of the energy release, nanoflares might be an important candidate for coronal heating; we seek to find that index. Methods: In this paper we employ a numerical three-dimensional (3D)-magnetohydrodynamic (MHD) simulation produced by the numerical code Bifrost, which enables us to look into smaller structures, and a new technique to identify the 3D heating events at a specific instant. The quantity we explore is the Joule heating, a term calculated directly by the code, which is explicitly correlated with the magnetic reconnection because it depends on the curl of the magnetic field. Results: We are able to identify 4136 events in a volume 24 × 24 × 9.5 Mm3 (I.e., 768 × 786 × 331 grid cells) of a specific snapshot. We find a powerlaw slope of the released energy per second equal to αP = 1.5 ± 0.02, and two powerlaw slopes of the identified volume equal to αV = 1.53 ± 0.03 and αV = 2.53 ± 0.22. The identified energy events do not represent all the released energy, but of the identified events, the total energy of the largest events

  5. A New Method for Coronal Magnetic Field Reconstruction

    Science.gov (United States)

    Yi, Sibaek; Choe, Gwang-Son; Cho, Kyung-Suk; Kim, Kap-Sung

    2017-08-01

    A precise way of coronal magnetic field reconstruction (extrapolation) is an indispensable tool for understanding of various solar activities. A variety of reconstruction codes have been developed so far and are available to researchers nowadays, but they more or less bear this and that shortcoming. In this paper, a new efficient method for coronal magnetic field reconstruction is presented. The method imposes only the normal components of magnetic field and current density at the bottom boundary to avoid the overspecification of the reconstruction problem, and employs vector potentials to guarantee the divergence-freeness. In our method, the normal component of current density is imposed, not by adjusting the tangential components of A, but by adjusting its normal component. This allows us to avoid a possible numerical instability that on and off arises in codes using A. In real reconstruction problems, the information for the lateral and top boundaries is absent. The arbitrariness of the boundary conditions imposed there as well as various preprocessing brings about the diversity of resulting solutions. We impose the source surface condition at the top boundary to accommodate flux imbalance, which always shows up in magnetograms. To enhance the convergence rate, we equip our code with a gradient-method type accelerator. Our code is tested on two analytical force-free solutions. When the solution is given only at the bottom boundary, our result surpasses competitors in most figures of merits devised by Schrijver et al. (2006). We have also applied our code to a real active region NOAA 11974, in which two M-class flares and a halo CME took place. The EUV observation shows a sudden appearance of an erupting loop before the first flare. Our numerical solutions show that two entwining flux tubes exist before the flare and their shackling is released after the CME with one of them opened up. We suggest that the erupting loop is created by magnetic reconnection between

  6. Reconstructed frontal and coronal cuts in computed tomography of the trunk

    International Nuclear Information System (INIS)

    Fochem, K.; Klumair, J.

    1982-01-01

    A comparison between the original coronally cuts and the reconstructed coronal cuts yielded basic information on the loss of quality by computed reconstruction of images. As for the trunk, only comparisons between the conventional linear tomography and computed frontal of trunk cuts are possible. A few examples will demonstrate that despite a considerable loss of quality, computed frontal cuts will supply additional information in certain cases. It is also shown that the reconstructed frontal cuts cannot replace conventional tomography. (orig.) [de

  7. A search for the origins of a possible coronal mass ejection in the low corona

    Science.gov (United States)

    Neupert, Werner M.

    1988-01-01

    Evidence for coronal and chromospheric precursors of a hypothesized coronal mass ejection is sought in OSO-7 observations of a filament eruption and the subsequent flare. Large-scale changes in the corona above the active region were clearly present for at least several minutes before the flare, culminating in the activation and eruption of two widely separated filaments; the eruption of one of the preexisting filaments initiated magnetic reconnections and energy releases in the low corona, generating the observed chromospheric flare.

  8. Self consistent MHD modeling of the solar wind from coronal holes with distinct geometries

    Science.gov (United States)

    Stewart, G. A.; Bravo, S.

    1995-01-01

    Utilizing an iterative scheme, a self-consistent axisymmetric MHD model for the solar wind has been developed. We use this model to evaluate the properties of the solar wind issuing from the open polar coronal hole regions of the Sun, during solar minimum. We explore the variation of solar wind parameters across the extent of the hole and we investigate how these variations are affected by the geometry of the hole and the strength of the field at the coronal base.

  9. CHROMOSPHERIC AND CORONAL WAVE GENERATION IN A MAGNETIC FLUX SHEATH

    International Nuclear Information System (INIS)

    Kato, Yoshiaki; Hansteen, Viggo; Gudiksen, Boris; Wedemeyer, Sven; Carlsson, Mats; Steiner, Oskar

    2016-01-01

    Using radiation magnetohydrodynamic simulations of the solar atmospheric layers from the upper convection zone to the lower corona, we investigate the self-consistent excitation of slow magneto-acoustic body waves (slow modes) in a magnetic flux concentration. We find that the convective downdrafts in the close surroundings of a two-dimensional flux slab “pump” the plasma inside it in the downward direction. This action produces a downflow inside the flux slab, which encompasses ever higher layers, causing an upwardly propagating rarefaction wave. The slow mode, excited by the adiabatic compression of the downflow near the optical surface, travels along the magnetic field in the upward direction at the tube speed. It develops into a shock wave at chromospheric heights, where it dissipates, lifts the transition region, and produces an offspring in the form of a compressive wave that propagates further into the corona. In the wake of downflows and propagating shock waves, the atmosphere inside the flux slab in the chromosphere and higher tends to oscillate with a period of ν ≈ 4 mHz. We conclude that this process of “magnetic pumping” is a most plausible mechanism for the direct generation of longitudinal chromospheric and coronal compressive waves within magnetic flux concentrations, and it may provide an important heat source in the chromosphere. It may also be responsible for certain types of dynamic fibrils.

  10. MAGNETIC FIELD STRUCTURES TRIGGERING SOLAR FLARES AND CORONAL MASS EJECTIONS

    International Nuclear Information System (INIS)

    Kusano, K.; Bamba, Y.; Yamamoto, T. T.; Iida, Y.; Toriumi, S.; Asai, A.

    2012-01-01

    Solar flares and coronal mass ejections, the most catastrophic eruptions in our solar system, have been known to affect terrestrial environments and infrastructure. However, because their triggering mechanism is still not sufficiently understood, our capacity to predict the occurrence of solar eruptions and to forecast space weather is substantially hindered. Even though various models have been proposed to determine the onset of solar eruptions, the types of magnetic structures capable of triggering these eruptions are still unclear. In this study, we solved this problem by systematically surveying the nonlinear dynamics caused by a wide variety of magnetic structures in terms of three-dimensional magnetohydrodynamic simulations. As a result, we determined that two different types of small magnetic structures favor the onset of solar eruptions. These structures, which should appear near the magnetic polarity inversion line (PIL), include magnetic fluxes reversed to the potential component or the nonpotential component of major field on the PIL. In addition, we analyzed two large flares, the X-class flare on 2006 December 13 and the M-class flare on 2011 February 13, using imaging data provided by the Hinode satellite, and we demonstrated that they conform to the simulation predictions. These results suggest that forecasting of solar eruptions is possible with sophisticated observation of a solar magnetic field, although the lead time must be limited by the timescale of changes in the small magnetic structures.

  11. Coronal mass ejections and their sheath regions in interplanetary space

    Science.gov (United States)

    Kilpua, Emilia; Koskinen, Hannu E. J.; Pulkkinen, Tuija I.

    2017-11-01

    Interplanetary coronal mass ejections (ICMEs) are large-scale heliospheric transients that originate from the Sun. When an ICME is sufficiently faster than the preceding solar wind, a shock wave develops ahead of the ICME. The turbulent region between the shock and the ICME is called the sheath region. ICMEs and their sheaths and shocks are all interesting structures from the fundamental plasma physics viewpoint. They are also key drivers of space weather disturbances in the heliosphere and planetary environments. ICME-driven shock waves can accelerate charged particles to high energies. Sheaths and ICMEs drive practically all intense geospace storms at the Earth, and they can also affect dramatically the planetary radiation environments and atmospheres. This review focuses on the current understanding of observational signatures and properties of ICMEs and the associated sheath regions based on five decades of studies. In addition, we discuss modelling of ICMEs and many fundamental outstanding questions on their origin, evolution and effects, largely due to the limitations of single spacecraft observations of these macro-scale structures. We also present current understanding of space weather consequences of these large-scale solar wind structures, including effects at the other Solar System planets and exoplanets. We specially emphasize the different origin, properties and consequences of the sheaths and ICMEs.

  12. FORMATION OF CORONAL HOLES ON THE ASHES OF ACTIVE REGIONS

    International Nuclear Information System (INIS)

    Karachik, Nina V.; Pevtsov, Alexei A.; Abramenko, Valentyna I.

    2010-01-01

    We investigate the formation of isolated non-polar coronal holes (CHs) on the remnants of decaying active regions (ARs) at the minimum/early ascending phase of sunspot activity. We follow the evolution of four bipolar ARs and measure several parameters of their magnetic fields including total flux, imbalance, and compactness. As regions decay, their leading and following polarities exhibit different dissipation rates: loose polarity tends to dissipate faster than compact polarity. As a consequence, we see a gradual increase in flux imbalance inside a dissipating bipolar region, and later a formation of a CH in place of more compact magnetic flux. Out of four cases studied in detail, two CHs had formed at the following polarity of the decaying bipolar AR, and two CHs had developed in place of the leading polarity field. All four CHs contain a significant fraction of magnetic field of their corresponding AR. Using potential field extrapolation, we show that the magnetic field lines of these CHs were closed on the polar CH at the North, which at the time of the events was in imbalance with the polar CH at the South. This topology suggests that the observed phenomenon may play an important role in transformation of toroidal magnetic field to poloidal field, which is a key step in transitioning from an old solar cycle to a new one. The timing of this observed transition may indicate the end of solar cycle 23 and the beginning of cycle 24.

  13. Areas of Polar Coronal Holes from 1996 Through 2010

    Science.gov (United States)

    Webber, Hess S. A.; Karna, N.; Pesnell, W. D.; Kirk, M. S.

    2014-01-01

    Polar coronal holes (PCHs) trace the magnetic variability of the Sun throughout the solar cycle. Their size and evolution have been studied as proxies for the global magnetic field. We present measurements of the PCH areas from 1996 through 2010, derived from an updated perimeter-tracing method and two synoptic-map methods. The perimeter tracing method detects PCH boundaries along the solar limb, using full-disk images from the SOlar and Heliospheric Observatory/Extreme ultraviolet Imaging Telescope (SOHO/EIT). One synoptic-map method uses the line-of-sight magnetic field from the SOHO/Michelson Doppler Imager (MDI) to determine the unipolarity boundaries near the poles. The other method applies thresholding techniques to synoptic maps created from EUV image data from EIT. The results from all three methods suggest that the solar maxima and minima of the two hemispheres are out of phase. The maximum PCH area, averaged over the methods in each hemisphere, is approximately 6 % during both solar minima spanned by the data (between Solar Cycles 22/23 and 23/24). The northern PCH area began a declining trend in 2010, suggesting a downturn toward the maximum of Solar Cycle 24 in that hemisphere, while the southern hole remained large throughout 2010.

  14. COMPARING CORONAL AND HELIOSPHERIC MAGNETIC FIELDS OVER SEVERAL SOLAR CYCLES

    Energy Technology Data Exchange (ETDEWEB)

    Koskela, J. S.; Virtanen, I. I.; Mursula, K., E-mail: jennimari.koskela@oulu.fi [University of Oulu, P.O. Box 3000, FI-90014 Oulu (Finland)

    2017-01-20

    Here we use the PFSS model and photospheric data from Wilcox Solar Observatory, SOHO /MDI, SDO/HMI, and SOLIS to compare the coronal field with heliospheric magnetic field measured at 1 au, compiled in the NASA/NSSDC OMNI 2 data set. We calculate their mutual polarity match and the power of the radial decay, p , of the radial field using different source surface distances and different number of harmonic multipoles. We find the average polarity match of 82% for the declining phase, 78%–79% for maxima, 76%–78% for the ascending phase, and 74%–76% for minima. On an average, the source surface of 3.25 R{sub S} gives the best polarity match. We also find strong evidence for solar cycle variation of the optimal source surface distance, with highest values (3.3 R{sub S}) during solar minima and lowest values (2.6 R{sub S}–2.7 R{sub S}) during the other three solar cycle phases. Raising the number of harmonic terms beyond 2 rarely improves the polarity match, showing that the structure of the HMF at 1 au is most of the time rather simple. All four data sets yield fairly similar polarity matches. Thus, polarity comparison is not affected by photospheric field scaling, unlike comparisons of the field intensity.

  15. KELVIN-HELMHOLTZ INSTABILITY OF A CORONAL STREAMER

    Energy Technology Data Exchange (ETDEWEB)

    Feng, L.; Gan, W. Q. [Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 210008 Nanjing (China); Inhester, B., E-mail: lfeng@pmo.ac.cn [Max-Planck-Institut fuer Sonnensystemforschung, Max-Planck-Str.2, D-37191 Katlenburg-Lindau (Germany)

    2013-09-10

    Shear-flow-driven instability can play an important role in energy transfer processes in coronal plasma. We present for the first time the observation of a kink-like oscillation of a streamer that is probably caused by the streaming kink-mode Kelvin-Helmholtz instability (KHI). The wave-like behavior of the streamer was observed by the Large Angle and Spectrometric Coronagraph Experiment C2 and C3 on board the SOlar and Heliospheric Observatory. The observed wave had a period of about 70-80 minutes, and its wavelength increased from 2 R{sub Sun} to 3 R{sub Sun} in about 1.5 hr. The phase speeds of its crests and troughs decreased from 406 {+-} 20 to 356 {+-} 31 km s{sup -1} during the event. Within the same heliocentric range, the wave amplitude also appeared to increase with time. We attribute the phenomena to the MHD KHI, which occurs at a neutral sheet in a fluid wake. The free energy driving the instability is supplied by the sheared flow and sheared magnetic field across the streamer plane. The plasma properties of the local environment of the streamer were estimated from the phase speed and instability threshold criteria.

  16. Sheath-accumulating Propagation of Interplanetary Coronal Mass Ejection

    Energy Technology Data Exchange (ETDEWEB)

    Takahashi, Takuya; Shibata, Kazunari, E-mail: takahasi@kusastro.kyoto-u.ac.jp [Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607–8471 (Japan)

    2017-03-10

    Fast interplanetary coronal mass ejections (ICMEs) are the drivers of strong space weather storms such as solar energetic particle events and geomagnetic storms. The connection between the space-weather-impacting solar wind disturbances associated with fast ICMEs at Earth and the characteristics of causative energetic CMEs observed near the Sun is a key question in the study of space weather storms, as well as in the development of practical space weather prediction. Such shock-driving fast ICMEs usually expand at supersonic speeds during the propagation, resulting in the continuous accumulation of shocked sheath plasma ahead. In this paper, we propose a “sheath-accumulating propagation” (SAP) model that describes the coevolution of the interplanetary sheath and decelerating ICME ejecta by taking into account the process of upstream solar wind plasma accumulation within the sheath region. Based on the SAP model, we discuss (1) ICME deceleration characteristics; (2) the fundamental condition for fast ICMEs at Earth; (3) the thickness of interplanetary sheaths; (4) arrival time prediction; and (5) the super-intense geomagnetic storms associated with huge solar flares. We quantitatively show that not only the speed but also the mass of the CME are crucial for discussing the above five points. The similarities and differences between the SAP model, the drag-based model, and the“snow-plow” model proposed by Tappin are also discussed.

  17. Spatially resolved X-ray spectra of coronal active regions

    International Nuclear Information System (INIS)

    Catura, R.C.; Acton, L.W.; Joki, E.G.; Rapley, C.G.; Culhane, J.L.

    1975-01-01

    X-ray spectra from a number of coronal active regions were obtained during ATM support rocket flights carried out by the Lockheed group on June 11 and December 19, 1973. Multi-grid collimators were used to provide fields of view of 40ins. diameter and 90ins. diameter for a number of scanning crystal spectrometers and a bent crystal spectrometer which employed a position sensitive proportional counter to register the diffracted spectrum. A solar image was produced on film and on a TV camera on board the rocket with the aid of a 1 A Hα filter. A small part of the X-ray collimator was used to generate a multiple spot diffraction pattern which was superimposed on the Hα image and the composite picture was transmitted to the ground. Pre-launch calibrations allowed the spot corresponding to the X-ray collimator axis to be identified and so the collimator pointing direction on the solar disc was controlled from the ground by means of commands sent to the rocket. (Auth.)

  18. 3D MHD MODELING OF TWISTED CORONAL LOOPS

    Energy Technology Data Exchange (ETDEWEB)

    Reale, F.; Peres, G. [Dipartimento di Fisica and Chimica, Università di Palermo, Piazza del Parlamento 1, I-90134 Palermo (Italy); Orlando, S. [INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, I-90134 Palermo (Italy); Guarrasi, M. [CINECA—Interuniversity consortium, via Magnanelli 6/3, I-40033, Casalecchio di Reno, Bologna (Italy); Mignone, A. [Dipartimento di Fisica Generale, Università di Torino, via Pietro Giuria 1, I-10125, Torino (Italy); Hood, A. W.; Priest, E. R., E-mail: fabio.reale@unipa.it [School of Mathematics and Statistics, University of St. Andrews, St. Andrews, KY16 9SS (United Kingdom)

    2016-10-10

    We perform MHD modeling of a single bright coronal loop to include the interaction with a non-uniform magnetic field. The field is stressed by random footpoint rotation in the central region and its energy is dissipated into heating by growing currents through anomalous magnetic diffusivity that switches on in the corona above a current density threshold. We model an entire single magnetic flux tube in the solar atmosphere extending from the high- β chromosphere to the low- β corona through the steep transition region. The magnetic field expands from the chromosphere to the corona. The maximum resolution is ∼30 km. We obtain an overall evolution typical of loop models and realistic loop emission in the EUV and X-ray bands. The plasma confined in the flux tube is heated to active region temperatures (∼3 MK) after ∼2/3 hr. Upflows from the chromosphere up to ∼100 km s{sup −1} fill the core of the flux tube to densities above 10{sup 9} cm{sup −3}. More heating is released in the low corona than the high corona and is finely structured both in space and time.

  19. CHROMOSPHERIC AND CORONAL WAVE GENERATION IN A MAGNETIC FLUX SHEATH

    Energy Technology Data Exchange (ETDEWEB)

    Kato, Yoshiaki; Hansteen, Viggo; Gudiksen, Boris; Wedemeyer, Sven; Carlsson, Mats [Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, NO-0315 Oslo (Norway); Steiner, Oskar, E-mail: yoshiaki.kato@astro.uio.no [Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, D-79104 Freiburg (Germany)

    2016-08-10

    Using radiation magnetohydrodynamic simulations of the solar atmospheric layers from the upper convection zone to the lower corona, we investigate the self-consistent excitation of slow magneto-acoustic body waves (slow modes) in a magnetic flux concentration. We find that the convective downdrafts in the close surroundings of a two-dimensional flux slab “pump” the plasma inside it in the downward direction. This action produces a downflow inside the flux slab, which encompasses ever higher layers, causing an upwardly propagating rarefaction wave. The slow mode, excited by the adiabatic compression of the downflow near the optical surface, travels along the magnetic field in the upward direction at the tube speed. It develops into a shock wave at chromospheric heights, where it dissipates, lifts the transition region, and produces an offspring in the form of a compressive wave that propagates further into the corona. In the wake of downflows and propagating shock waves, the atmosphere inside the flux slab in the chromosphere and higher tends to oscillate with a period of ν ≈ 4 mHz. We conclude that this process of “magnetic pumping” is a most plausible mechanism for the direct generation of longitudinal chromospheric and coronal compressive waves within magnetic flux concentrations, and it may provide an important heat source in the chromosphere. It may also be responsible for certain types of dynamic fibrils.

  20. Production planning and coronal stop deletion in spontaneous speech

    Directory of Open Access Journals (Sweden)

    James Tanner

    2017-06-01

    Full Text Available Many phonological processes can be affected by segmental context spanning word boundaries, which often lead to variable outcomes. This paper tests the idea that some of this variability can be explained by reference to production planning. We examine coronal stop deletion (CSD, a variable process conditioned by preceding and upcoming phonological context, in a corpus of spontaneous British English speech, as a means of investigating a number of variables associated with planning: Prosodic boundary strength, word frequency, conditional probability of the following word, and speech rate. From the perspective of production planning, (1 prosodic boundaries should affect deletion rate independently of following context; (2 given the locality of production planning, the effect of the following context should decrease at stronger prosodic boundaries; and (3 other factors affecting planning scope should modulate the effect of upcoming phonological material above and beyond the modulating effect of prosodic boundaries. We build a statistical model of CSD realization, using pause length as a quantitative proxy for boundary strength, and find support for these predictions. These findings are compatible with the hypothesis that the locality of production planning constrains variability in speech production, and have practical implications for work on CSD and other variable processes.

  1. Coronal mass ejections and their sheath regions in interplanetary space

    Directory of Open Access Journals (Sweden)

    Emilia Kilpua

    2017-11-01

    Full Text Available Abstract Interplanetary coronal mass ejections (ICMEs are large-scale heliospheric transients that originate from the Sun. When an ICME is sufficiently faster than the preceding solar wind, a shock wave develops ahead of the ICME. The turbulent region between the shock and the ICME is called the sheath region. ICMEs and their sheaths and shocks are all interesting structures from the fundamental plasma physics viewpoint. They are also key drivers of space weather disturbances in the heliosphere and planetary environments. ICME-driven shock waves can accelerate charged particles to high energies. Sheaths and ICMEs drive practically all intense geospace storms at the Earth, and they can also affect dramatically the planetary radiation environments and atmospheres. This review focuses on the current understanding of observational signatures and properties of ICMEs and the associated sheath regions based on five decades of studies. In addition, we discuss modelling of ICMEs and many fundamental outstanding questions on their origin, evolution and effects, largely due to the limitations of single spacecraft observations of these macro-scale structures. We also present current understanding of space weather consequences of these large-scale solar wind structures, including effects at the other Solar System planets and exoplanets. We specially emphasize the different origin, properties and consequences of the sheaths and ICMEs.

  2. A numerical study of two interacting coronal mass ejections

    Directory of Open Access Journals (Sweden)

    J. M. Schmidt

    2004-06-01

    Full Text Available The interaction in the solar wind between two coronal mass ejections (CMEs is investigated using numerical simulations. We show that the nature of the interaction depends on whether the CME magnetic structures interact, but in all cases the result is an equilisation of the speed of the two CMEs. In the absence of magnetic interaction, the forward shock of the faster trailing CME interacts with the slow leading CME, and accelerates it. When the two CMEs have magnetic fields with the same sense of rotation, magnetic reconnection occurs between the two CMEs, leading to the formation of a single magnetic structure: in the most extreme cases, one CME "eats" the other. When the senses of rotation are opposite, reconnection does not occur, but the CMEs collide in a highly non-elastic manner, again forming a single structure. The possibility of enhanced particle acceleration in such processes is assessed. The presence of strong magnetic reconnection provides excellent opportunities for the acceleration of thermal particles, which then form a seed population for further acceleration at the CME shocks. The presence of a large population of seed particles will thus lead to an overall increase in energetic particle fluxes, as suggested by some observations.

  3. Sheath-accumulating Propagation of Interplanetary Coronal Mass Ejection

    International Nuclear Information System (INIS)

    Takahashi, Takuya; Shibata, Kazunari

    2017-01-01

    Fast interplanetary coronal mass ejections (ICMEs) are the drivers of strong space weather storms such as solar energetic particle events and geomagnetic storms. The connection between the space-weather-impacting solar wind disturbances associated with fast ICMEs at Earth and the characteristics of causative energetic CMEs observed near the Sun is a key question in the study of space weather storms, as well as in the development of practical space weather prediction. Such shock-driving fast ICMEs usually expand at supersonic speeds during the propagation, resulting in the continuous accumulation of shocked sheath plasma ahead. In this paper, we propose a “sheath-accumulating propagation” (SAP) model that describes the coevolution of the interplanetary sheath and decelerating ICME ejecta by taking into account the process of upstream solar wind plasma accumulation within the sheath region. Based on the SAP model, we discuss (1) ICME deceleration characteristics; (2) the fundamental condition for fast ICMEs at Earth; (3) the thickness of interplanetary sheaths; (4) arrival time prediction; and (5) the super-intense geomagnetic storms associated with huge solar flares. We quantitatively show that not only the speed but also the mass of the CME are crucial for discussing the above five points. The similarities and differences between the SAP model, the drag-based model, and the“snow-plow” model proposed by Tappin are also discussed.

  4. Regarding the detectability and measurement of coronal mass ejections

    Directory of Open Access Journals (Sweden)

    Howard Timothy A.

    2015-01-01

    Full Text Available In this review I discuss the problems associated with the detection and measurement of coronal mass ejections (CMEs. CMEs are important phenomena both scientifically, as they play a crucial role in the evolution of the solar corona, and technologically, as their impact with the Earth leads to severe space weather activity in the form of magnetic storms. I focus on the observation of CMEs using visible white light imagers (coronagraphs and heliospheric imagers, as they may be regarded as the binding agents between different datasets and different models that are used to reconstruct them. Our ability to accurately measure CMEs observed by these imagers is hampered by many factors, from instrumental to geometrical to physical. Following a brief review of the history of CME observation and measurement, I explore the impediments to our ability to measure them and describe possible means for which we may be able to mitigate those impediments. I conclude with a discussion of the claim that we have reached the limit of the information that we can extract from the current generation of white light imagers, and discuss possible ways forward regarding future instrument capabilities.

  5. Coronal and local thermodynamic equilibriums in a hollow cathode discharge

    International Nuclear Information System (INIS)

    Zheng Xutao

    2005-01-01

    A characteristic two-section profile of excited-state populations is observed in a hollow cathode discharge and is explained by coexistence of the coronal equilibrium (CE) and the local thermodynamic equilibrium (LTE). At helium pressure 0.1 Torr and cathode current 200-300 mA, vacuum ultraviolet radiations from He I 1snp 1 P (n=2-16) and He II np 2 P (n=2-14) are resolved with a 2.2-M McPherson spectrometer. Relative populations of these states are deduced from the discrete line intensities and are plotted against energy levels. For both the He I and He II series, as energy level increases, populations of high-n (n>10) states are found to decrease much more quickly than low-n (n<7) populations. While low-n populations are described with the CE dominated by direct electron-impact excitations, high-n populations are fitted with the LTE to calculate the population temperatures of gas atoms and ions. Validities of the CE and LTE in different n-ranges are considered on the competition between radiative decays of the excited states and their collisions with gas atoms. (author)

  6. GLOBAL ENERGETICS OF SOLAR FLARES. IV. CORONAL MASS EJECTION ENERGETICS

    International Nuclear Information System (INIS)

    Aschwanden, Markus J.

    2016-01-01

    This study entails the fourth part of a global flare energetics project, in which the mass m cme , kinetic energy E kin , and the gravitational potential energy E grav of coronal mass ejections (CMEs) is measured in 399 M and X-class flare events observed during the first 3.5 years of the Solar Dynamics Observatory (SDO) mission, using a new method based on the EUV dimming effect. EUV dimming is modeled in terms of a radial adiabatic expansion process, which is fitted to the observed evolution of the total emission measure of the CME source region. The model derives the evolution of the mean electron density, the emission measure, the bulk plasma expansion velocity, the mass, and the energy in the CME source region. The EUV dimming method is truly complementary to the Thomson scattering method in white light, which probes the CME evolution in the heliosphere at r ≳ 2 R ⊙ , while the EUV dimming method tracks the CME launch in the corona. We compare the CME parameters obtained in white light with the LASCO/C2 coronagraph with those obtained from EUV dimming with the Atmospheric Imaging Assembly onboard the SDO for all identical events in both data sets. We investigate correlations between CME parameters, the relative timing with flare parameters, frequency occurrence distributions, and the energy partition between magnetic, thermal, nonthermal, and CME energies. CME energies are found to be systematically lower than the dissipated magnetic energies, which is consistent with a magnetic origin of CMEs.

  7. Coronal Mass Ejections: Models and Their Observational Basis

    Directory of Open Access Journals (Sweden)

    P. F. Chen

    2011-04-01

    Full Text Available Coronal mass ejections (CMEs are the largest-scale eruptive phenomenon in the solar system, expanding from active region-sized nonpotential magnetic structure to a much larger size. The bulk of plasma with a mass of ∼10^11 – 10^13 kg is hauled up all the way out to the interplanetary space with a typical velocity of several hundred or even more than 1000 km s^-1, with a chance to impact our Earth, resulting in hazardous space weather conditions. They involve many other much smaller-sized solar eruptive phenomena, such as X-ray sigmoids, filament/prominence eruptions, solar flares, plasma heating and radiation, particle acceleration, EIT waves, EUV dimmings, Moreton waves, solar radio bursts, and so on. It is believed that, by shedding the accumulating magnetic energy and helicity, they complete the last link in the chain of the cycling of the solar magnetic field. In this review, I try to explicate our understanding on each stage of the fantastic phenomenon, including their pre-eruption structure, their triggering mechanisms and the precursors indicating the initiation process, their acceleration and propagation. Particular attention is paid to clarify some hot debates, e.g., whether magnetic reconnection is necessary for the eruption, whether there are two types of CMEs, how the CME frontal loop is formed, and whether halo CMEs are special.

  8. Understanding the Physical Nature of Coronal "EIT Waves".

    Science.gov (United States)

    Long, D M; Bloomfield, D S; Chen, P F; Downs, C; Gallagher, P T; Kwon, R-Y; Vanninathan, K; Veronig, A M; Vourlidas, A; Vršnak, B; Warmuth, A; Žic, T

    2017-01-01

    For almost 20 years the physical nature of globally propagating waves in the solar corona (commonly called "EIT waves") has been controversial and subject to debate. Additional theories have been proposed over the years to explain observations that did not agree with the originally proposed fast-mode wave interpretation. However, the incompatibility of observations made using the Extreme-ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory with the fast-mode wave interpretation was challenged by differing viewpoints from the twin Solar Terrestrial Relations Observatory spacecraft and data with higher spatial and temporal resolution from the Solar Dynamics Observatory . In this article, we reexamine the theories proposed to explain EIT waves to identify measurable properties and behaviours that can be compared to current and future observations. Most of us conclude that the so-called EIT waves are best described as fast-mode large-amplitude waves or shocks that are initially driven by the impulsive expansion of an erupting coronal mass ejection in the low corona.

  9. FGFR2c-mediated ERK-MAPK activity regulates coronal suture development

    Science.gov (United States)

    Pfaff, Miles J.; Xue, Ke; Li, Li; Horowitz, Mark C.; Steinbacher, Derek M.; Eswarakumar, Jacob V.P.

    2017-01-01

    Fibroblast growth factor receptor 2 (FGFR2) signaling is critical for proper craniofacial development. A gain-of-function mutation in the 2c splice variant of the receptor’s gene is associated with Crouzon syndrome, which is characterized by craniosynostosis, the premature fusion of one or more of the cranial vault sutures, leading to craniofacial maldevelopment. Insight into the molecular mechanism of craniosynostosis has identified the ERK-MAPK signaling cascade as a critical regulator of suture patency. The aim of this study is to investigate the role of FGFR2c-induced ERK-MAPK activation in the regulation of coronal suture development. Loss-of-function and gain-of-function Fgfr2c mutant mice have overlapping phenotypes, including coronal synostosis and craniofacial dysmorphia. In vivo analysis of coronal sutures in loss-of-function and gain-of-function models demonstrated fundamentally different pathogenesis underlying coronal suture synostosis. Calvarial osteoblasts from gain-of-function mice demonstrated enhanced osteoblastic function and maturation with concomitant increase in ERK-MAPK activation. In vitro inhibition with the ERK protein inhibitor U0126 mitigated ERK protein activation levels with a concomitant reduction in alkaline phosphatase activity. This study identifies FGFR2c-mediated ERK-MAPK signaling as a key mediator of craniofacial growth and coronal suture development. Furthermore, our results solve the apparent paradox between loss-of-function and gain-of-function FGFR2c mutants with respect to coronal suture synostosis. PMID:27034231

  10. Additional merit of coronal STIR imaging for MR imaging of lumbar spine

    Directory of Open Access Journals (Sweden)

    Ranjana Gupta

    2015-01-01

    Full Text Available Introduction: Back pain is a common clinical problem and is the frequent complaint for referral of lumbar spine magnetic resonance imaging (MRI. Coronal short tau inversion recovery sequence (STIR can provide diagnostically significant information in small percentage of patients. Materials and Methods: MRI examinations of a total of 350 patients were retrospectively included in the study. MR sequences were evaluated in two settings. One radiologist evaluated sagittal and axial images only, while another radiologist evaluated all sequences, including coronal STIR sequence. After recording the diagnoses, we compared the MRI findings in two subsets of patients to evaluate additional merit of coronal STIR imaging. Results: With addition of coronal STIR imaging, significant findings were observed in 24 subjects (6.8%. Twenty-one of these subjects were considered to be normal on other sequences and in three subjects diagnosis was changed with the addition of coronal STIR. Additional diagnoses on STIR included sacroiliitis, sacroiliac joint degenerative disease, sacral stress/insufficiency fracture/Looser′s zones, muscular sprain and atypical appendicitis. Conclusion: Coronal STIR imaging can provide additional diagnoses in a small percentage of patients presenting for lumbar spine MRI for back pain. Therefore, it should be included in the routine protocol for MR imaging of lumbar spine.

  11. Diagnostics of Coronal Magnetic Fields through the Hanle Effect in UV and IR Lines

    Energy Technology Data Exchange (ETDEWEB)

    Raouafi, Nour E. [The John Hopkins University Applied Physics Laboratory, Laurel, MD (United States); Riley, Pete [Predictive Science Inc., San Diego, CA (United States); Gibson, Sarah [High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO (United States); Fineschi, Silvano [The Astrophysical Observatory of Turin, National Institute for Astrophysics, Turin (Italy); Solanki, Sami K., E-mail: noureddine.raouafi@jhuapl.edu [Max-Planck-Institut für Sonnensystemforschung, Göttingen (Germany); School of Space Research, Kyung Hee University, Yongin, South (Korea, Republic of)

    2016-06-22

    The plasma thermodynamics in the solar upper atmosphere, particularly in the corona, are dominated by the magnetic field, which controls the flow and dissipation of energy. The relative lack of knowledge of the coronal vector magnetic field is a major handicap for progress in coronal physics. This makes the development of measurement methods of coronal magnetic fields a high priority in solar physics. The Hanle effect in the UV and IR spectral lines is a largely unexplored diagnostic. We use magnetohydrodynamic (MHD) simulations to study the magnitude of the signal to be expected for typical coronal magnetic fields for selected spectral lines in the UV and IR wavelength ranges, namely the H i Ly-α and the He i 10,830 Å lines. We show that the selected lines are useful for reliable diagnosis of coronal magnetic fields. The results show that the combination of polarization measurements of spectral lines with different sensitivities to the Hanle effect may be most appropriate for deducing coronal magnetic properties from future observations.

  12. Are interplanetary magnetic clouds manifestations of coronal transients at 1 AU

    International Nuclear Information System (INIS)

    Wilson, R.M.; Hildner, E.

    1984-01-01

    Using proxy data for the occurrence of those mass ejections from the solar corona which are directed earthward, we investigate the association between the post-1970 interplanetary magnetic clouds of Klein and Burlaga (1982) and coronal mass ejections. The evidence linking magnetic clouds following shocks with coronal mass ejections is striking; six of nine clouds observed at Earth were preceded an appropriate time earlier by meter-wave type II radio bursts indicative of coronal shock waves and coronal mass ejections occurring near central meridian. During the selected control periods when no clouds were detected near Earth, the only type II bursts reported were associated with solar activity near the limbs. Where the proxy solar data to be sought are not so clearly suggested, that is, for clouds preceding interaction regions and clouds within cold magnetic enhancements, the evidence linking the clouds and coronal mass ejections is not as clear; proxy data usually suggest many candidate mass-ejection events for each cloud. Overall, the data are consistent with and support the hypothesis suggested by Klein and Burlaga that magnetic clouds observed with spacecraft at 1 AU are manifestations of solar coronal mass ejection transients. (orig.)

  13. Solar Coronal Loops Associated with Small-scale Mixed Polarity Surface Magnetic Fields

    Energy Technology Data Exchange (ETDEWEB)

    Chitta, L. P.; Peter, H.; Solanki, S. K.; Barthol, P.; Gandorfer, A.; Gizon, L.; Hirzberger, J.; Riethmüller, T. L.; Noort, M. van [Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, D-37077 Göttingen (Germany); Rodríguez, J. Blanco [Grupo de Astronomía y Ciencias del Espacio, Universidad de Valencia, E-46980 Paterna, Valencia (Spain); Iniesta, J. C. Del Toro; Suárez, D. Orozco [Instituto de Astrofísica de Andalucía (CSIC), Apartado de Correos 3004, E-18080 Granada (Spain); Schmidt, W. [Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, D-79104 Freiburg (Germany); Pillet, V. Martínez [National Solar Observatory, 3665 Discovery Drive, Boulder, CO 80303 (United States); Knölker, M., E-mail: chitta@mps.mpg.de [High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307-3000 (United States)

    2017-03-01

    How and where are coronal loops rooted in the solar lower atmosphere? The details of the magnetic environment and its evolution at the footpoints of coronal loops are crucial to understanding the processes of mass and energy supply to the solar corona. To address the above question, we use high-resolution line-of-sight magnetic field data from the Imaging Magnetograph eXperiment instrument on the Sunrise balloon-borne observatory and coronal observations from the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory of an emerging active region. We find that the coronal loops are often rooted at the locations with minor small-scale but persistent opposite-polarity magnetic elements very close to the larger dominant polarity. These opposite-polarity small-scale elements continually interact with the dominant polarity underlying the coronal loop through flux cancellation. At these locations we detect small inverse Y-shaped jets in chromospheric Ca ii H images obtained from the Sunrise Filter Imager during the flux cancellation. Our results indicate that magnetic flux cancellation and reconnection at the base of coronal loops due to mixed polarity fields might be a crucial feature for the supply of mass and energy into the corona.

  14. Solar Coronal Loops Associated with Small-scale Mixed Polarity Surface Magnetic Fields

    International Nuclear Information System (INIS)

    Chitta, L. P.; Peter, H.; Solanki, S. K.; Barthol, P.; Gandorfer, A.; Gizon, L.; Hirzberger, J.; Riethmüller, T. L.; Noort, M. van; Rodríguez, J. Blanco; Iniesta, J. C. Del Toro; Suárez, D. Orozco; Schmidt, W.; Pillet, V. Martínez; Knölker, M.

    2017-01-01

    How and where are coronal loops rooted in the solar lower atmosphere? The details of the magnetic environment and its evolution at the footpoints of coronal loops are crucial to understanding the processes of mass and energy supply to the solar corona. To address the above question, we use high-resolution line-of-sight magnetic field data from the Imaging Magnetograph eXperiment instrument on the Sunrise balloon-borne observatory and coronal observations from the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory of an emerging active region. We find that the coronal loops are often rooted at the locations with minor small-scale but persistent opposite-polarity magnetic elements very close to the larger dominant polarity. These opposite-polarity small-scale elements continually interact with the dominant polarity underlying the coronal loop through flux cancellation. At these locations we detect small inverse Y-shaped jets in chromospheric Ca ii H images obtained from the Sunrise Filter Imager during the flux cancellation. Our results indicate that magnetic flux cancellation and reconnection at the base of coronal loops due to mixed polarity fields might be a crucial feature for the supply of mass and energy into the corona.

  15. Does Tibial Slope Affect Perception of Coronal Alignment on a Standing Anteroposterior Radiograph?

    Science.gov (United States)

    Schwartz, Adam J; Ravi, Bheeshma; Kransdorf, Mark J; Clarke, Henry D

    2017-07-01

    A standing anteroposterior (AP) radiograph is commonly used to evaluate coronal alignment following total knee arthroplasty (TKA). The impact of coronal alignment on TKA outcomes is controversial, perhaps due to variability in imaging and/or measurement technique. We sought to quantify the effect of image rotation and tibial slope on coronal alignment. Using a standard extramedullary tibial alignment guide, 3 cadaver legs were cut to accept a tibial tray at 0°, 3°, and 7° of slope. A computed tomography scan of the entire tibia was obtained for each specimen to confirm neutral coronal alignment. Images were then obtained at progressive 10° intervals of internal and external rotation up to 40° maximum in each direction. Images were then randomized and 5 blinded TKA surgeons were asked to determine coronal alignment. Continuous data values were transformed to categorical data (neutral [0], valgus [L], and varus [R]). Each 10° interval of external rotation of a 7° sloped tibial cut (or relative internal rotation of a tibial component viewed in the AP plane) resulted in perception of an additional 0.75° of varus. The slope of the proximal tibia bone cut should be taken into account when measuring coronal alignment on a standing AP radiograph. Copyright © 2017 Elsevier Inc. All rights reserved.

  16. Combined Ulysses Solar Wind and SOHO Coronal Observations of Several West Limb Coronal Mass Ejections. Appendix 8

    Science.gov (United States)

    Funsten, H. O.; Gosling, J. T.; Riley, P.; St.Cyr, O. C.; Forsyth, R. J.; Howard, R. A.; Schwenn, R.

    2001-01-01

    From October 1996 to January 1997, Ulysses was situated roughly above the west limb of the Sun as observed from Earth at a heliocentric distance of about 4.6 AU and a latitude of about 25 deg. This presents the first opportunity to compare Solar and Heliospheric Observatory (SOHO) limb observations of coronal mass ejections (CMEs) directly with their solar wind counterparts far from the Sun using the Ulysses data. During this interval, large eruptive events were observed above the west limb of the Sun by the Large Angle Spectrometric Coronagraph (LASCO) on SOHO on October 5, November 28, and December 21-25, 1996. Using the combined plasma and magnetic field data from Ulysses, the October 5 event was clearly identified by several distinguishing signatures as a CME. The November 28 event was also identified as a CME that trailed fast ambient solar wind, although it was identified only by an extended interval of counterstreaming suprathermal electrons. The December 21 event was apparently characterized by a six-day interval of nearly radial field and a plasma rarefaction. For the numerous eruptive events observed by the LASCO coronagraph during December 23-25, Ulysses showed no distinct, CMEs, perhaps because of intermingling of two or more of the eruptive events. By mapping the Ulysses observations back in time to the Sun assuming a constant flow speed, we have identified intervals of plasma that were accelerated or decelerated between the LASCO and Ulysses observations.

  17. Coronal Mass Ejections: a Summary of Recent Results

    Science.gov (United States)

    Gopalswamy, Nat; Davila, J. M.

    2010-01-01

    Coronal mass ejections (CMEs) have been recognized as the most energetic phenomenon in the heliosphere, deriving their energy from the stressed magnetic fields on the Sun. This paper highlights some of the recent results on CMEs obtained from the Solar and Heliospheric Observatory (SOHO) and the Solar Terrestrial Relations Observatory (STEREO) missions. The summary of the talk follows. SOHO observations revealed that the CME rate is almost a factor of two larger than previously thought and varied with the solar activity cycle in a complex way (e.g., high-latitude CMEs occurred in great abundance during the solar maximum years). CMEs were found to interact with other CMEs as well as with other large-scale structures (coronal holes), resulting in deflections and additional particle acceleration. STEREO observations have confirmed the three-dimensional nature of CMEs and the shocks surrounding them. The EUV signatures (flare arcades, corona) dimming, filament eruption, and EUV waves) associated with CMEs have become vital in the identification of solar sources from which CMEs erupt. CMEs with speeds exceeding the characteristic speeds of the corona and the interplanetary medium drive shocks, which produce type II radio bursts. The wavelength range of type II bursts depends on the CME kinetic energy: type II bursts with emission components at all wavelengths (metric to kilometric) are due to CMEs of the highest kinetic energy. Some CMEs, as fast as 1600 km/s do not produce type II bursts, while slow CMEs (400 km/s) occasionally produce type II bursts. These observations can be explained as the variation in the ambient flow speed (solar wind) and the Alfven speed. Not all CME-driven shocks produce type II bursts because either they are subcritical or do not have the appropriate geometry. The same shocks that produce type II bursts also produce solar energetic particles (SEPs), whose release near the Sun seems to be delayed with respect to the onset of type II bursts

  18. Upper gastrointestinal bleeding in a Brazilian hospital: a retrospective study of endoscopic records Sangramento digestivo alto em um hospital brasileiro: estudo retrospectivo de registros endoscópicos

    Directory of Open Access Journals (Sweden)

    Cyrla ZALTMAN

    2002-04-01

    attributed to a higher prevalence of variceal bleeding and underlying liver disease.Racional - A hemorragia digestiva alta é complicação comum e grave da maioria das doenças do trato gastrointestinal superior. A endoscopia tem papel fundamental no diagnóstico e no tratamento da hemorragia digestiva, mas os dados epidemiológicos a esse respeito ainda são precários em nosso meio. Objetivos - Determinar as características clínicas, a acurácia endoscópica, a eficácia do tratamento e a evolução clínica dos pacientes admitidos no setor de endoscopia digestiva do Hospital Universitário da Universidade Federal do Rio de Janeiro, Rio de Janeiro, RJ, com sangramento digestivo alto. Pacientes e Métodos - Estudo retrospectivo de registros consecutivos de pacientes com hemorragia digestiva alta submetidos a endoscopia de urgência, em período de 2 anos. Resultados - A maioria dos pacientes era do sexo masculino (68.7% com idade média de 54,5 ± 17,5 anos. O sítio de sangramento foi identificado em 75.6% dos pacientes. A acurácia diagnóstica da endoscopia foi maior quando realizada nas primeiras 24 horas do início do sangramento e quando da presença de hematêmese. A úlcera péptica foi a principal causa de hemorragia digestiva alta (35%. A prevalência de sangramento varicoso (20,45% indica freqüência alta de hepatopatia subjacente. O tratamento endoscópico foi realizado em 23,86% dos pacientes. Hemostasia permanente foi alcançada em 86% dos pacientes após a primeira intervenção endoscópica e em 62,5% dos pacientes após ressangramento. Cirurgia de emergência foi raramente necessária. A quantidade de unidades de sangue utilizada foi em média 1,44 ± 1,99 por paciente. O tempo médio de internação hospitalar foi de 7,71 ± 12,2 dias. Ressangramento foi observado em 9,1% dos pacientes. A taxa de mortalidade de 15,34% foi significativamente relacionada com a presença de doença hepática prévia. Conclusões - A acurácia diagnóstica foi

  19. Ulysses' rapid crossing of the polar coronal hole boundary

    International Nuclear Information System (INIS)

    McComas, D.J.; Riley, P.; Gosling, J.T.; Balogh, A.; Forsyth, R.

    1998-01-01

    The Ulysses spacecraft crossed from the slow dense solar wind characteristic of the solar streamer belt into the fast, less dense flow from the northern polar coronal hole over a very short interval (several days) in late March 1995. The spacecraft, which was at 1.35 AU and ∼19 degree north heliographic latitude, moving northward in its orbit, remained in the fast solar wind from then through summer 1996. This boundary crossing is unique in that the combination of the spacecraft motion and rotation of the structure past the spacecraft caused Ulysses to move smoothly and completely from one regime into the other. In this study we examine this crossing in detail. The crossing is marked by a region of enhanced pressure, typical of stream interaction regions, which extends ∼2x10 7 km across. We find that the transition between the slow and fast regimes occurs on several temporal, and hence spatial, scales. On the shortest scale ( 4 km) the stream interface is a tangential discontinuity where the proton and core electron densities and ion and electron pressures all drop while the magnetic pressure jumps to maintain a rough pressure balance. The alpha to proton ratio also jumps across the stream interface to reach the comparatively constant polar hole value of ∼4.3%. On larger scales (a few x10 6 km) the proton and alpha temperatures rise to their high-speed wind values. Finally, on the largest scale (∼10 8 km) the solar wind speed ramps up from ∼400kms -1 to ∼750kms -1 , typical of polar hole flows. While it seems likely that the stream interface maps back to a sharp boundary near the Sun, the large region of increasing flow speed suggests that there is also an extended gradient in solar wind source speed close to the Sun. copyright 1998 American Geophysical Union

  20. Predicting Coronal Mass Ejections Using Machine Learning Methods

    Science.gov (United States)

    Bobra, M. G.; Ilonidis, S.

    2016-04-01

    Of all the activity observed on the Sun, two of the most energetic events are flares and coronal mass ejections (CMEs). Usually, solar active regions that produce large flares will also produce a CME, but this is not always true. Despite advances in numerical modeling, it is still unclear which circumstances will produce a CME. Therefore, it is worthwhile to empirically determine which features distinguish flares associated with CMEs from flares that are not. At this time, no extensive study has used physically meaningful features of active regions to distinguish between these two populations. As such, we attempt to do so by using features derived from (1) photospheric vector magnetic field data taken by the Solar Dynamics Observatory’s Helioseismic and Magnetic Imager instrument and (2) X-ray flux data from the Geostationary Operational Environmental Satellite’s X-ray Flux instrument. We build a catalog of active regions that either produced both a flare and a CME (the positive class) or simply a flare (the negative class). We then use machine-learning algorithms to (1) determine which features distinguish these two populations, and (2) forecast whether an active region that produces an M- or X-class flare will also produce a CME. We compute the True Skill Statistic, a forecast verification metric, and find that it is a relatively high value of ∼0.8 ± 0.2. We conclude that a combination of six parameters, which are all intensive in nature, will capture most of the relevant information contained in the photospheric magnetic field.

  1. Understanding Solar Coronal Heating through Atomic and Plasma Physics Experiments

    Science.gov (United States)

    Savin, Daniel Wolf; Arthanayaka, Thusitha; Bose, Sayak; Hahn, Michael; Beiersdorfer, Peter; Brown, Gregory V.; Gekelman, Walter; Vincena, Steve

    2017-08-01

    Recent solar observations suggest that the Sun's corona is heated by Alfven waves that dissipate at unexpectedly low heights in the corona. These observations raise a number of questions. Among them are the problems of accurately quantifying the energy flux of the waves and that of describing the physical mechanism that leads to the wave damping. We are performing laboratory experiments to address both of these issues.The energy flux depends on the electron density, which can be measured spectroscopically. However, spectroscopic density diagnostics have large uncertainties, because they depend sensitively on atomic collisional excitation, de-excitation, and radiative transition rates for multiple atomic levels. Essentially all of these data come from theory and have not been experimentally validated. We are conducting laboratory experiments using the electron beam ion trap (EBIT) at Lawrence Livermore National Laboratory that will provide accurate empirical calibrations for spectroscopic density diagnostics and which will also help to guide theoretical calculations.The observed rapid wave dissipation is likely due to inhomogeneities in the plasma that drive flows and currents at small length scales where energy can be more efficiently dissipated. This may take place through gradients in the Alfvén speed along the magnetic field, which causes wave reflection and generates turbulence. Alternatively, gradients in the Alfvén speed across the field can lead to dissipation through phase-mixing. Using the Large Plasma Device (LAPD) at the University of California Los Angeles, we are studying both of these dissipation mechanisms in the laboratory in order to understand their potential roles in coronal heating.

  2. Evolution of coronal mass ejections and their heliospheric imprints

    International Nuclear Information System (INIS)

    Rollett, T.

    2014-01-01

    Coronal mass ejections (CMEs) are the most powerful eruptions on the Sun and can reach speeds up to more than 3000 km/s. CMEs are the most important drivers of space weather and can cause geomagnetic storms when interacting with the Earth magnetosphere.The evolution and propagation of CMEs in interplanetary space is still not well understood. Interactions with the solar wind as well as other CMEs make accurate forecasting of arrival times difficult. The Constrained Harmonic Mean (CHM) method combines remote sensing white light data of STEREO/HI with in situ data and offers the possibility to derive kinematical profiles for any segment along the CME front to study its evolution in interplanetary space. We studied the influence of the ambient solar wind flow on the propagation behavior for three CME events. The kinematics revealed by the CHM method were compared to the simulated background solar wind. We found that CMEs are highly dependent on speed variations of the ambient medium. The CHM method was tested by analyzing a simulated CME as observed by STEREO/HI. After applying the CHM method, the resulting CME kinematics were compared to the real kinematics of the simulated CME. We found that the CHM method works best for small separation angles between the spacecraft. A case study of a fast CME that has been remotely observed by both STEREO/HI and in situ measured by four spacecraft at different heliocentric distances is also presented. Using this high number of in situ detections and the two side views we derived different speed profiles for the two different segments of the same CME causing a deformation of the overall structure of the CME. The studies presented show the effects of different influences of the ambient solar wind on the CME evolution. Interaction of CMEs with the solar wind or other CMEs lead to disturbances of the speed as well as the shape of CMEs, affecting their arrival time and their geoeffectivity. (author) [de

  3. Intermittency in MHD turbulence and coronal nanoflares modelling

    Directory of Open Access Journals (Sweden)

    P. Veltri

    2005-01-01

    Full Text Available High resolution numerical simulations, solar wind data analysis, and measurements at the edges of laboratory plasma devices have allowed for a huge progress in our understanding of MHD turbulence. The high resolution of solar wind measurements has allowed to characterize the intermittency observed at small scales. We are now able to set up a consistent and convincing view of the main properties of MHD turbulence, which in turn constitutes an extremely efficient tool in understanding the behaviour of turbulent plasmas, like those in solar corona, where in situ observations are not available. Using this knowledge a model to describe injection, due to foot-point motions, storage and dissipation of MHD turbulence in coronal loops, is built where we assume strong longitudinal magnetic field, low beta and high aspect ratio, which allows us to use the set of reduced MHD equations (RMHD. The model is based on a shell technique in the wave vector space orthogonal to the strong magnetic field, while the dependence on the longitudinal coordinate is preserved. Numerical simulations show that injected energy is efficiently stored in the loop where a significant level of magnetic and velocity fluctuations is obtained. Nonlinear interactions give rise to an energy cascade towards smaller scales where energy is dissipated in an intermittent fashion. Due to the strong longitudinal magnetic field, dissipative structures propagate along the loop, with the typical speed of the Alfvén waves. The statistical analysis on the intermittent dissipative events compares well with all observed properties of nanoflare emission statistics. Moreover the recent observations of non thermal velocity measurements during flare occurrence are well described by the numerical results of the simulation model. All these results naturally emerge from the model dynamical evolution without any need of an ad-hoc hypothesis.

  4. Coronal Mass Ejection Data Clustering and Visualization of Decision Trees

    Science.gov (United States)

    Ma, Ruizhe; Angryk, Rafal A.; Riley, Pete; Filali Boubrahimi, Soukaina

    2018-05-01

    Coronal mass ejections (CMEs) can be categorized as either “magnetic clouds” (MCs) or non-MCs. Features such as a large magnetic field, low plasma-beta, and low proton temperature suggest that a CME event is also an MC event; however, so far there is neither a definitive method nor an automatic process to distinguish the two. Human labeling is time-consuming, and results can fluctuate owing to the imprecise definition of such events. In this study, we approach the problem of MC and non-MC distinction from a time series data analysis perspective and show how clustering can shed some light on this problem. Although many algorithms exist for traditional data clustering in the Euclidean space, they are not well suited for time series data. Problems such as inadequate distance measure, inaccurate cluster center description, and lack of intuitive cluster representations need to be addressed for effective time series clustering. Our data analysis in this work is twofold: clustering and visualization. For clustering we compared the results from the popular hierarchical agglomerative clustering technique to a distance density clustering heuristic we developed previously for time series data clustering. In both cases, dynamic time warping will be used for similarity measure. For classification as well as visualization, we use decision trees to aggregate single-dimensional clustering results to form a multidimensional time series decision tree, with averaged time series to present each decision. In this study, we achieved modest accuracy and, more importantly, an intuitive interpretation of how different parameters contribute to an MC event.

  5. Birth, life, and death of a solar coronal plume

    Energy Technology Data Exchange (ETDEWEB)

    Pucci, Stefano; Romoli, Marco [Department of Physics and Astronomy, University of Firenze, Largo Enrico Fermi 5, I-50125 Firenze (Italy); Poletto, Giannina [INAF-Arcetri Astrophysical Observatory, Largo Enrico Fermi 5, I-50125 Firenze (Italy); Sterling, Alphonse C., E-mail: stpucci@arcetri.astro.it [Space Science Office, NASA/MSFC, Huntsville, AL 35812 (United States)

    2014-10-01

    We analyze a solar polar-coronal-hole (CH) plume over its entire ≈40 hr lifetime, using high-resolution Solar Dynamic Observatory Atmospheric Imaging Assembly (AIA) data. We examine (1) the plume's relationship to a bright point (BP) that persists at its base, (2) plume outflows and their possible contribution to the solar wind mass supply, and (3) the physical properties of the plume. We find that the plume started ≈2 hr after the BP first appeared and became undetectable ≈1 hr after the BP disappeared. We detected radially moving radiance variations from both the plume and from interplume regions, corresponding to apparent outflow speeds ranging over ≈(30-300) km s{sup –1} with outflow velocities being higher in the 'cooler' AIA 171 Å channel than in the 'hotter' 193 Å and 211 Å channels, which is inconsistent with wave motions; therefore, we conclude that the observed radiance variations represent material outflows. If they persist into the heliosphere and plumes cover ≈10% of a typical CH area, these flows could account for ≈50% of the solar wind mass. From a differential emission measure analysis of the AIA images, we find that the average electron temperature of the plume remained approximately constant over its lifetime, at T {sub e} ≈ 8.5 × 10{sup 5} K. Its density, however, decreased with the age of the plume, being about a factor of three lower when the plume faded compared to when it was born. We conclude that the plume died due to a density reduction rather than to a temperature decrease.

  6. Differential Rotation via Tracking of Coronal Bright Points.

    Science.gov (United States)

    McAteer, James; Boucheron, Laura E.; Osorno, Marcy

    2016-05-01

    The accurate computation of solar differential rotation is important both as a constraint for, and evidence towards, support of models of the solar dynamo. As such, the use of Xray and Extreme Ultraviolet bright points to elucidate differential rotation has been studied in recent years. In this work, we propose the automated detection and tracking of coronal bright points (CBPs) in a large set of SDO data for re-evaluation of solar differential rotation and comparison to other results. The big data aspects, and high cadence, of SDO data mitigate a few issues common to detection and tracking of objects in image sequences and allow us to focus on the use of CBPs to determine differential rotation. The high cadence of the data allows to disambiguate individual CBPs between subsequent images by allowing for significant spatial overlap, i.e., by the fact that the CBPs will rotate a short distance relative to their size. The significant spatial overlap minimizes the effects of incorrectly detected CBPs by reducing the occurrence of outlier values of differential rotation. The big data aspects of the data allows to be more conservative in our detection of CBPs (i.e., to err on the side of missing CBPs rather than detecting extraneous CBPs) while still maintaining statistically larger populations over which to study characteristics. The ability to compute solar differential rotation through the automated detection and tracking of a large population of CBPs will allow for further analyses such as the N-S asymmetry of differential rotation, variation of differential rotation over the solar cycle, and a detailed study of the magnetic flux underlying the CBPs.

  7. PREDICTING CORONAL MASS EJECTIONS USING MACHINE LEARNING METHODS

    Energy Technology Data Exchange (ETDEWEB)

    Bobra, M. G.; Ilonidis, S. [W.W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305 (United States)

    2016-04-20

    Of all the activity observed on the Sun, two of the most energetic events are flares and coronal mass ejections (CMEs). Usually, solar active regions that produce large flares will also produce a CME, but this is not always true. Despite advances in numerical modeling, it is still unclear which circumstances will produce a CME. Therefore, it is worthwhile to empirically determine which features distinguish flares associated with CMEs from flares that are not. At this time, no extensive study has used physically meaningful features of active regions to distinguish between these two populations. As such, we attempt to do so by using features derived from (1) photospheric vector magnetic field data taken by the Solar Dynamics Observatory ’s Helioseismic and Magnetic Imager instrument and (2) X-ray flux data from the Geostationary Operational Environmental Satellite’s X-ray Flux instrument. We build a catalog of active regions that either produced both a flare and a CME (the positive class) or simply a flare (the negative class). We then use machine-learning algorithms to (1) determine which features distinguish these two populations, and (2) forecast whether an active region that produces an M- or X-class flare will also produce a CME. We compute the True Skill Statistic, a forecast verification metric, and find that it is a relatively high value of ∼0.8 ± 0.2. We conclude that a combination of six parameters, which are all intensive in nature, will capture most of the relevant information contained in the photospheric magnetic field.

  8. Methods of Temperature and Emission Measure Determination of Coronal Loops

    Science.gov (United States)

    Cirtain, J. W.; Schmelz, J. T.; Martens, P. C. H.

    2002-05-01

    Recent observational results from both SOHO-EIT and TRACE indicate that coronal loops are isothermal along their length (axially). These results are obtained from a narrowband filter ratio method that assumes that the plasma is isothermal along the line of sight (radially). However, these temperatures vary greatly from those derived from differential emission measure (DEM) curves produced from spectral lines recorded by SOHO-CDS. The DEM results indicate that the loops are neither axially nor radially isothermal. This discrepancy was investigated by Schmelz et al. (2001). They chose pairs of iron lines from the same CDS data set to mimic the EIT and TRACE loop results. Ratios of different lines gave different temperatures, indicating that the plasma was not radially isothermal. In addition the results indicated that the loop was axially isothermal, even though the DEM analysis of the same data showed this result to be false. Here we have analyzed the EIT data for the CDS loop published by Schmelz et al. (2001). We took the ratios of the 171-to-195 and 195-to-284 filter data, and made temperature maps of the loop. The results indicate that the loop is axially isothermal, but different temperatures were found for each pair of filters. Both ratio techniques force the resultant temperature to lie within the range where the response functions (for filters) or the emissivity functions (for lines) overlap; isothermal loops are therefore a byproduct of the analysis. This conclusion strengthens support for the idea that temperature and emission measure results from filter ratio methods may be misleading or even drastically wrong. This research was funded in part by the NASA/TRACE MODA grant for Montana State University. Solar physics research at the University of Memphis is supported by NASA grant NAG5-9783.

  9. Fault lines in forensic medical toxicology in Ireland exposed through replies of pathologists and coroners to anonymous questionnaires.

    Science.gov (United States)

    Tormey, William P; Borovickova, Ingrid; Moore, Tara M

    2014-01-01

    The attitudes and experiences of pathologists and coroners to the provision of biochemical forensic toxicology in the Republic of Ireland were determined using separate questionnaires to each group anonymously. Replies were received from 36/88 (41%) of pathologists and 19/71 (27%) of coroners. 37% of coroners considered that histopathologists give an adequate opinion in forensic toxicology yet 58% of pathologists reported that they did not have adequate access to expert medical interpretative toxicological opinion. For drug-drug interactions and metabolic diseases, 69% of pathologists were unhappy with the processes and 68% of coroner replies did not know if vitreous samples were used appropriately. There is a clear requirement for retraining of coroners and for the appointment of medical toxicology expertise to improve the quality of service for coroners.

  10. Root canal adhesive filling in dogs' teeth with or without coronal restoration: a histopathological evaluation.

    Science.gov (United States)

    Leonardo, Mario Roberto; Barnett, Frederick; Debelian, Gilberto J; de Pontes Lima, Regina Karla; Bezerra da Silva, Léa Assed

    2007-11-01

    The purpose of this study was to evaluate in vivo the response of the periradicular tissues after endodontic treatment and root filling with Epiphany/Resilon (Penntron Clinical Technologies, LLC, Wallingford, CT) or gutta percha and new Sealapex (SybronEndo, Glendora, CA) in dogs' teeth with or without coronal restoration. Teeth without coronal restorations were used to assess the influence of continuous exposure to the oral environment on the periradicular tissues. Sixty root canals with vital pulps in three dogs were instrumented and obturated in a single session and randomly assigned to one of four groups as follows. group 1: root canal filling with Epiphany/Resilon with coronal restoration, group 2: root canal filling with Sealapex sealer and gutta percha with restoration, group 3: root canal filling with Epiphany/Resilon without restoration, and group 4: root canal filling with Sealapex sealer and gutta percha without coronal restoration. After 90 days, the animals were euthanized, and the maxillas and mandibles were removed and submitted for histologic processing. Longitudinal sections were obtained and stained with hematoxylin and eosin, Mallory's trichrome, and Brown and Brenn stains and examined under light microscopy. There were significant differences found between the four groups (p < 0.05). The results showed that roots canals filled with Epiphany/Resilon, with coronal restoration, had significantly less periradicular inflammation than roots canals filled with gutta percha and Sealapex, with coronal restoration (p = 0.021). No significant difference was observed in the intensity of inflammation between roots canals filled with Epiphany/Resilon with no restoration and roots filled with gutta percha and Sealapex with restoration (p = 0.269). Roots canals filled with gutta percha and Sealapex sealer without coronal restoration showed the greatest degree of periradicular inflammation.

  11. Decision-making in a death investigation: Emotion, families and the coroner.

    Science.gov (United States)

    Tait, Gordon; Carpenter, Belinda; Quadrelli, Carol; Barnes, Michael

    2016-03-01

    The role of the coroner in common law countries such as Australia, England, Canada and New Zealand is to preside over death investigations where there is uncertainty as to the manner of death, a need to identify the deceased, a death of unknown cause, or a violent or unnatural death. The vast majority of these deaths are not suspicious and thus require coroners to engage with grieving families who have been thrust into a legal process through the misfortune of a loved one's sudden or unexpected death. In this research, 10 experienced coroners discussed how they negotiated the grief and trauma evident in a death investigation. In doing so, they articulated two distinct ways in which legal officers engaged with emotions, which are also evident in the literature. The first engages the script of judicial dispassion, articulating a hierarchical relationship between reason and emotion, while the second introduces an ethic of care via the principles of therapeutic jurisprudence, and thus offers a challenge to the role of emotion in the personae of the professional judicial officer. By using Hochschild's work on the sociology of emotions, this article discusses the various ways in which coroners manage the emotion of a death investigation through emotion work. While emotional distance may be an understandable response by coroners to the grief and trauma experienced by families and directed at cleaner coronial decision-making, the article concludes that coroners may be better served by offering emotions such as sympathy, consideration and compassion directly to the family in those situations where families are struggling to accept, or are resistant to, coroners' decisions.

  12. Remaking the medico-legal scene: a social history of the late-Victorian coroner in Oxford.

    Science.gov (United States)

    Hurren, Elizabeth T

    2010-04-01

    There have been wide-ranging debates about medicine and the law encapsulated in the figure of the coroner in Victorian England. Recently the historical literature on coroners has been enriched by macro-studies. Despite this important research, the social lives of coroners and their daily interactions remain relatively neglected in standard historical accounts. This article redresses that issue by examining the working life of the coroner for Oxford during the late-Victorian era. Edward Law Hussey kept very detailed records of his time in office as coroner. New research material makes it feasible to trace his professional background, from doctor of the sick poor, to hospital house surgeon and then busy coroner. His career trajectory, personal interactions, and professional disputes, provide an important historical prism illuminating contemporary debates that occupied coroners in their working lives. Hussey tried to improve his medico-legal reach and the public image of his coroner's office by reducing infanticide rates, converting a public mortuary, and acquiring a proper coroner's court. His campaigns had limited success because the social scene in which he worked was complicated by the dominance of health and welfare agencies that resented his role as an expanding arm of the Victorian information state.

  13. Future space missions and ground observatory for measurements of coronal magnetic fields

    Science.gov (United States)

    Fineschi, Silvano; Gibson, Sarah; Bemporad, Alessandro; Zhukov, Andrei; Damé, Luc; Susino, Roberto; Larruquert, Juan

    2016-07-01

    This presentation gives an overview of the near-future perspectives for probing coronal magnetism from space missions (i.e., SCORE and ASPIICS) and ground-based observatory (ESCAPE). Spectro-polarimetric imaging of coronal emission-lines in the visible-light wavelength-band provides an important diagnostics tool of the coronal magnetism. The interpretation in terms of Hanle and Zeeman effect of the line-polarization in forbidden emission-lines yields information on the direction and strength of the coronal magnetic field. As study case, this presentation will describe the Torino Coronal Magnetograph (CorMag) for the spectro-polarimetric observation of the FeXIV, 530.3 nm, forbidden emission-line. CorMag - consisting of a Liquid Crystal (LC) Lyot filter and a LC linear polarimeter. The CorMag filter is part of the ESCAPE experiment to be based at the French-Italian Concordia base in Antarctica. The linear polarization by resonance scattering of coronal permitted line-emission in the ultraviolet (UV)can be modified by magnetic fields through the Hanle effect. Space-based UV spectro-polarimeters would provide an additional tool for the disgnostics of coronal magnetism. As a case study of space-borne UV spectro-polarimeters, this presentation will describe the future upgrade of the Sounding-rocket Coronagraphic Experiment (SCORE) to include new generation, high-efficiency UV polarizer with the capability of imaging polarimetry of the HI Lyman-α, 121.6 nm. SCORE is a multi-wavelength imager for the emission-lines, HeII 30.4 nm and HI 121.6 nm, and visible-light broad-band emission of the polarized K-corona. SCORE has flown successfully in 2009. The second lauch is scheduled in 2016. Proba-3 is the other future solar mission that would provide the opportunity of diagnosing the coronal magnetic field. Proba-3 is the first precision formation-flying mission to launched in 2019). A pair of satellites will fly together maintaining a fixed configuration as a 'large rigid

  14. Ruptura do ligamento cruzado em cães: estudo retrospectivo da reconstituição com fascia lata Managment of cruciate ligament rupture in dogs: a retrospective study fascia lata autograft

    Directory of Open Access Journals (Sweden)

    Paulo Iamaguti

    1998-12-01

    Full Text Available Trata-se de um estudo retrospectivo de 35 casos de ruptura de ligamento cruzado atendidos pelo Serviço de Cirurgia de Pequenos Animais da FMVZ-UNESP-Campus de Botucatu, no período janeiro de 1991 a junho de 1997. Os cães foram submetidos à técnica de PAATSAMA (1952, modificada para reconstituição do ligamento cruzado, que consistiu na passagem do retalho de fascia lata através da articulação do joelho e fixação no côndilo medial da tíbia e epicôndilo medial do fêmur. Pelos resultados obtidos, concluiu-se que esta técnica permite boa estabilização das superfícies articulares, com trans e pós operatório sem complicações, e permite recuperação completa da capacidade funcional do membro afetado.This is a retrospectivo study of 35 cases of cruciate ligament rupture, submitted to Small Animal Surgery Service at FMVZ - UNESP - Compus de Botucatu, from January, 1991 to June, 1997. The dogs underwent a modifica techniquefor reconstitution of the cruciate ligament. A flap of fascia lata was placed through the stifle joint andfixed at the medial condyle ofthe tíbia and the medial condyle of the femur. Results showed that this technique was simple and satisfactory, with no trans and post operative complications. The dogs totally recovered the function of the limbs in ali cases submitted to surgery.

  15. Evidence for the Magnetic Breakout Model in an Equatorial Coronal-hole Jet

    Science.gov (United States)

    Kumar, Pankaj; Karpen, Judith T.; Antiochos, Spiro K.; Wyper, Peter F.; DeVore, C. Richard; DeForest, Craig E.

    2018-02-01

    Small, impulsive jets commonly occur throughout the solar corona, but are especially visible in coronal holes. Evidence is mounting that jets are part of a continuum of eruptions that extends to much larger coronal mass ejections and eruptive flares. Because coronal-hole jets originate in relatively simple magnetic structures, they offer an ideal testbed for theories of energy buildup and release in the full range of solar eruptions. We analyzed an equatorial coronal-hole jet observed by the Solar Dynamics Observatory (SDO)/AIA on 2014 January 9 in which the magnetic-field structure was consistent with the embedded-bipole topology that we identified and modeled previously as an origin of coronal jets. In addition, this event contained a mini-filament, which led to important insights into the energy storage and release mechanisms. SDO/HMI magnetograms revealed footpoint motions in the primary minority-polarity region at the eruption site, but show negligible flux emergence or cancellation for at least 16 hr before the eruption. Therefore, the free energy powering this jet probably came from magnetic shear concentrated at the polarity inversion line within the embedded bipole. We find that the observed activity sequence and its interpretation closely match the predictions of the breakout jet model, strongly supporting the hypothesis that the breakout model can explain solar eruptions on a wide range of scales.

  16. Mode Conversion of a Solar Extreme-ultraviolet Wave over a Coronal Cavity

    Energy Technology Data Exchange (ETDEWEB)

    Zong, Weiguo [Key Laboratory of Space Weather, National Center for Space Weather, China Meteorological Administration, Beijing 100081 (China); Dai, Yu, E-mail: ydai@nju.edu.cn [Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210023 (China)

    2017-01-10

    We report on observations of an extreme-ultraviolet (EUV) wave event in the Sun on 2011 January 13 by Solar Terrestrial Relations Observatory and Solar Dynamics Observatory in quadrature. Both the trailing edge and the leading edge of the EUV wave front in the north direction are reliably traced, revealing generally compatible propagation velocities in both perspectives and a velocity ratio of about 1/3. When the wave front encounters a coronal cavity near the northern polar coronal hole, the trailing edge of the front stops while its leading edge just shows a small gap and extends over the cavity, meanwhile getting significantly decelerated but intensified. We propose that the trailing edge and the leading edge of the northward propagating wave front correspond to a non-wave coronal mass ejection component and a fast-mode magnetohydrodynamic wave component, respectively. The interaction of the fast-mode wave and the coronal cavity may involve a mode conversion process, through which part of the fast-mode wave is converted to a slow-mode wave that is trapped along the magnetic field lines. This scenario can reasonably account for the unusual behavior of the wave front over the coronal cavity.

  17. Image-based reconstruction of the Newtonian dynamics of solar coronal ejecta

    Science.gov (United States)

    Uritsky, Vadim M.; Thompson, Barbara J.

    2016-10-01

    We present a new methodology for analyzing rising and falling dynamics of unstable coronal material as represented by high-cadence SDO AIA images. The technique involves an adaptive spatiotemporal tracking of propagating intensity gradients and their characterization in terms of time-evolving areas swept out by the position vector originated from the Sun disk center. The measured values of the areal velocity and acceleration are used to obtain quantitative information on the angular momentum and acceleration along the paths of the rising and falling coronal plasma. In the absence of other forces, solar gravitation results in purely ballistic motions consistent with the Kepler's second law; non-central forces such as the Lorentz force introduce non-zero torques resulting in more complex motions. The developed algorithms enable direct evaluation of the line-of-sight component of the net torque applied to a unit mass of the ejected coronal material which is proportional to the image-plane projection of the observed areal acceleration. The current implementation of the method cannot reliably distinguish torque modulations caused by the coronal force field from those imposed by abrupt changes of plasma mass density and nontrivial projection effects. However, it can provide valid observational constraints on the evolution of large-scale unstable magnetic topologies driving major solar-coronal eruptions as demonstrated in the related talk by B. Thompson et al.

  18. Influência da técnica anestésica nas alterações hemodinâmicas no transplante renal: estudo retrospectivo Influencia de la técnica anestésica en las alteraciones hemodinámicas en el transplante renal: estudio retrospectivo Influence of the anesthetic technique on the hemodynamic changes in renal transplantation: a retrospective study

    Directory of Open Access Journals (Sweden)

    Eunice Sizue Hirata

    2009-04-01

    Full Text Available JUSTIFICATIVA E OBJETIVOS: Sucesso no transplante renal (Tx depende do tipo de doador, da duração da isquemia fria e de parâmetros hemodinâmicos na reperfusão. O objetivo desta pesquisa foi analisar a técnica anestésica, a incidência de alterações cardiovasculares e a ocorrência de diurese no período perioperatório dos Tx realizados na UNICAMP. MÉTODO: Avaliou-se retrospectivamente Tx de adultos realizados entre janeiro de 2005 e abril de 2006. Consideraram-se dados demográficos, exames laboratoriais pré-operatórios, técnicas e agentes anestésicos, hidratação, parâmetros hemodinâmicos, emprego de aminas vasoativas, presença de diurese e complicações intra-operatórias, com análise comparativa entre os subgrupos formados conforme a técnica anestésica empregada. Foram usados na análise estatística o teste t de Student (paramétricos, Mann-Whitney (não paramétricos, teste do Qui-quadrado e Exato de Fisher para comparação de proporções e análise multivariada. RESULTADOS: Estudaram-se 92 pacientes, 59 com anestesia geral (AG e 33 anestesia geral associada à peridural (AG + Peri, 42 receberam rim de doadores vivos e 50 de falecidos. Não houve diferença (p > 0,05 na maioria dos parâmetros pré-operatórios estudados, exceção feita à origem do enxerto (82% AG + Peri receberam rins de doador falecido. A alteração cardiovascular mais frequente foi hipotensão arterial (30% AG e 48% AG + Peri, p JUSTIFICATIVA Y OBJETIVOS: El éxito en el transplante renal (Tx depende del tipo de donador, de la duración de la isquemia fría y de los parámetros hemodinámicos en la reperfusión. El objetivo de esta investigación fue analizar la técnica anestésica, la incidencia de alteraciones cardiovasculares y el aparecimiento de diuresis en el período perioperatorio de los Tx realizados en la UNICAMP. MÉTODO: Se evaluó retrospectivamente Tx de adultos realizados entre enero de 2005 y abril de 2006. Se tuvieron en cuenta los datos demográficos, los exámenes laboratoriales preoperatorios, técnicas y agentes anestésicos, hidratación, parámetros hemodinámicos, el uso de aminas vasoactivas, la presencia de diuresis y complicaciones intraoperatorias, con análisis comparativo entre los subgrupos formados conforme a la técnica anestésica empleada. Se usaron en el análisis estadístico el test t de Student (paramétricos, Mann-Whitney (no paramétricos, test del Cui-cuadrado y Exacto de Fisher para la comparación de proporciones y análisis multivariada. RESULTADOS: Se estudiaron 92 pacientes, 59 con anestesia general (AG y 33 anestesia general asociada a la epidural (AG + Peri, 42 recibieron riñones de donantes vivos y 50 de fallecidos. No hubo diferencia (p BACKGROUND AND OBJECTIVES: The success of renal transplantation (Tx depends on the type of donor, length of cold ischemia, and hemodynamic parameters on reperfusion. The objective of this study was to analyze the anesthetic technique, the incidence of cardiovascular changes, and the presence of postoperative diuresis of Tx performed at UNICAMP. METHODS: Renal transplantation of adults performed from January 2005 and April 2006 were evaluated retrospectively. Demographic data, preoperative laboratorial exams, anesthetic techniques and agents, hydration, hemodynamic parameters, use of vasoactive amines, presence of a diuresis, and intraoperative complications were evaluated, and comparative analysis between the subgroups, formed according to the anesthetic technique, was undertaken. The Student t test (parametric, Mann-Whitney test (non-parametric, Chi-square test and Fisher Exact test for comparison of proportions and multivariate analysis were used. RESULTS: Ninety-two patients were evaluated; 59 underwent general anesthesia (GA and 33 underwent general anesthesia associated with epidural block (GA + Epi; 42 patients received live-donor transplants and 50 from dead donors. Most preoperative parameters analyzed did not show statistically significant differences (p > 0.05, except for the origin of the graft (82% of GA + Epi received dead donor kidneys. Hypotension (30% GA and 48% GA + Epi, p < 0.05 was the most frequent cardiovascular change. The hydration regimen did not differ between both groups (86.7± 30.2 mL.kg-1 GA and 94.8 ± 21.8 mL.kg-1 GA+Epi, p = 0.38. Dead donor grafts were more commonly associated with hemodynamic instability and worse prognosis for the immediate function of the graft, p < 0.01 and 0.01, respectively. Hydration of 80 mL.kg-1 was associated with the presence of diuresis (OR = 2.94, CI 95% 1.00-8.32. CONCLUSIONS: General anesthesia associated or not with epidural block was the anesthetic technique used. Hypotension was the most common hemodynamic change. Live-donor graft and volume of hydration of 80 mL.kg-1 of NS favored diuresis.

  19. El creciente campo de los Estudios Sensoriales

    Directory of Open Access Journals (Sweden)

    David Howes

    2014-09-01

    Full Text Available Este ensayo presenta una breve descripción acerca del giro sensorial en la investigación contemporánea, y propone algunas perspectivas de trabajo para futuras investigaciones. Esta labor no pretende ser exhaustiva y, más bien, busca indicar las principales tendencias en este campo. El ensayo, en su primera parte, ofrece una mirada general sobre la aparición y el desarrollo de la historia y la antropología de los sentidos. En la segunda parte, la atención se concentra en cómo el campo de los estudios sensoriales puede ser, de otro lado, conceptualizado como compuesto de cultura visual, cultura auditiva (o estudios del sonido, cultura del olfato, cultura del gusto y cultura del tacto. Se ofrece una explicación acerca de la génesis de estas divisiones. Posteriormente, se presenta una visión general de algunas cuestiones claves en los estudios sensoriales, como la pregunta por el número de los sentidos y la relación entre orden sensorial y orden social. El ensayo concluye con ocho proposiciones para los estudios sensoriales.

  20. El creciente campo de los Estudios Sensoriales

    Directory of Open Access Journals (Sweden)

    David Howes

    2014-08-01

    Full Text Available Este ensayo presenta una breve descripción acerca del giro sensorial en la investigación contemporánea, y propone algunas perspectivas de trabajo para futurasinvestigaciones. Esta labor no pretende ser exhaustiva y, más bien, busca indicar las principales tendencias en este campo. El ensayo, en su primera parte, ofrece una mirada general sobre la aparición y el desarrollo de la historia y la antropología de los sentidos. En la segunda parte, la atención se concentra en cómo el campo de los estudios sensoriales puede ser, de otro lado, conceptualizado como compuesto de cultura visual, cultura auditiva (o estudios del sonido, cultura del olfato, cultura del gusto y cultura del tacto. Se ofrece una explicación acerca de la génesis de estas divisiones. Posteriormente,se presenta una visión general de algunas cuestiones claves en los estudios sensoriales, como la pregunta por el número de los sentidos y la relación entre orden sensorial y orden social. El ensayo concluye con ocho proposiciones para los estudios sensoriales.

  1. ON SUN-TO-EARTH PROPAGATION OF CORONAL MASS EJECTIONS

    International Nuclear Information System (INIS)

    Liu, Ying D.; Luhmann, Janet G.; Möstl, Christian; Bale, Stuart D.; Lin, Robert P.; Lugaz, Noé; Davies, Jackie A.

    2013-01-01

    We investigate how coronal mass ejections (CMEs) propagate through, and interact with, the inner heliosphere between the Sun and Earth, a key question in CME research and space weather forecasting. CME Sun-to-Earth kinematics are constrained by combining wide-angle heliospheric imaging observations, interplanetary radio type II bursts, and in situ measurements from multiple vantage points. We select three events for this study, the 2012 January 19, 23, and March 7 CMEs. Different from previous event studies, this work attempts to create a general picture for CME Sun-to-Earth propagation and compare different techniques for determining CME interplanetary kinematics. Key results are obtained concerning CME Sun-to-Earth propagation: (1) the Sun-to-Earth propagation of fast CMEs can be approximately formulated into three phases: an impulsive acceleration, then a rapid deceleration, and finally a nearly constant speed propagation (or gradual deceleration); (2) the CMEs studied here are still accelerating even after the flare maximum, so energy must be continuously fed into the CME even after the time of the maximum heating and radiation has elapsed in the corona; (3) the rapid deceleration, presumably due to interactions with the ambient medium, mainly occurs over a relatively short timescale following the acceleration phase; and (4) CME-CME interactions seem a common phenomenon close to solar maximum. Our comparison between different techniques (and data sets) has important implications for CME observations and their interpretations: (1) for the current cases, triangulation assuming a compact CME geometry is more reliable than triangulation assuming a spherical front attached to the Sun for distances below 50-70 solar radii from the Sun, but beyond about 100 solar radii we would trust the latter more; (2) a proper treatment of CME geometry must be performed in determining CME Sun-to-Earth kinematics, especially when the CME propagation direction is far away from the

  2. Spatial variation of AIA coronal Fourier power spectra

    Science.gov (United States)

    Ireland, J.; Mcateer, R. T. J.

    2015-12-01

    We describe a study of the spatial distribution of the properties of the Fourier power spectrum of time-series of AIA 171Å and 193Å data. The area studied includes examples of physically different components of the corona, such as coronal moss, a sunspot, quiet Sun and fan loop footpoints. We show that a large fraction of the power spectra are well modeled by a power spectrum that behaves like a power law f-n (n>0)at lower frequencies f, dropping to a constant value at higher frequencies. We also show that there are areas where the power spectra are better described by the above power spectrum model, plus a narrow band oscillatory feature, centered in the 3-5 minute oscillation range. These narrow-band spectral features are thought to be due to the propagation of oscillations from lower down in solar atmosphere to hotter. This allows us to produce maps of large areas of the corona showing where the propagation from one waveband to another does and does not occur. This is an important step in understanding wave propagation in different layers in the corona. We also show the 171Å and 193Å power spectrum power law indices are correlated, with 171Å power law indices in the range n = 1.8 to 2.8, and 193Å power law indices n = 2 to 3.5 approximately. Maps of the power law index show that different ranges of values of the power law indices occur in spatially contiguous parts of the corona, indicating that local spatial structure may play a role in defining the power law index value. Taken with our previous result from Ireland et al. (2015) that physically different parts of the corona have different mean values of the power law index, this new result strongly suggests that the same mechanism producing the observed power law power spectrum is operating everywhere across the corona. We discuss the nanoflare hypothesis as a possible explanation of these observations.

  3. Flare Prediction Using Photospheric and Coronal Image Data

    Science.gov (United States)

    Jonas, E.; Shankar, V.; Bobra, M.; Recht, B.

    2016-12-01

    We attempt to forecast M-and X-class solar flares using a machine-learning algorithm and five years of image data from both the Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA) instruments aboard the Solar Dynamics Observatory. HMI is the first instrument to continuously map the full-disk photospheric vector magnetic field from space (Schou et al., 2012). The AIA instrument maps the transition region and corona using various ultraviolet wavelengths (Lemen et al., 2012). HMI and AIA data are taken nearly simultaneously, providing an opportunity to study the entire solar atmosphere at a rapid cadence. Most flare forecasting efforts described in the literature use some parameterization of solar data - typically of the photospheric magnetic field within active regions. These numbers are considered to capture the information in any given image relevant to predicting solar flares. In our approach, we use HMI and AIA images of solar active regions and a deep convolutional kernel network to predict solar flares. This is effectively a series of shallow-but-wide random convolutional neural networks stacked and then trained with a large-scale block-weighted least squares solver. This algorithm automatically determines which patterns in the image data are most correlated with flaring activity and then uses these patterns to predict solar flares. Using the recently-developed KeystoneML machine learning framework, we construct a pipeline to process millions of images in a few hours on commodity cloud computing infrastructure. This is the first time vector magnetic field images have been combined with coronal imagery to forecast solar flares. This is also the first time such a large dataset of solar images, some 8.5 terabytes of images that together capture over 3000 active regions, has been used to forecast solar flares. We evaluate our method using various flare prediction windows defined in the literature (e.g. Ahmed et al., 2013) and a novel per

  4. Quantifying and containing the curse of high resolution coronal imaging

    Directory of Open Access Journals (Sweden)

    V. Delouille

    2008-10-01

    Full Text Available Future missions such as Solar Orbiter (SO, InterHelioprobe, or Solar Probe aim at approaching the Sun closer than ever before, with on board some high resolution imagers (HRI having a subsecond cadence and a pixel area of about (80 km2 at the Sun during perihelion. In order to guarantee their scientific success, it is necessary to evaluate if the photon counts available at these resolution and cadence will provide a sufficient signal-to-noise ratio (SNR. For example, if the inhomogeneities in the Quiet Sun emission prevail at higher resolution, one may hope to locally have more photon counts than in the case of a uniform source. It is relevant to quantify how inhomogeneous the quiet corona will be for a pixel pitch that is about 20 times smaller than in the case of SoHO/EIT, and 5 times smaller than TRACE. We perform a first step in this direction by analyzing and characterizing the spatial intermittency of Quiet Sun images thanks to a multifractal analysis. We identify the parameters that specify the scale-invariance behavior. This identification allows next to select a family of multifractal processes, namely the Compound Poisson Cascades, that can synthesize artificial images having some of the scale-invariance properties observed on the recorded images. The prevalence of self-similarity in Quiet Sun coronal images makes it relevant to study the ratio between the SNR present at SoHO/EIT images and in coarsened images. SoHO/EIT images thus play the role of "high resolution" images, whereas the "low-resolution" coarsened images are rebinned so as to simulate a smaller angular resolution and/or a larger distance to the Sun. For a fixed difference in angular resolution and in Spacecraft-Sun distance, we determine the proportion of pixels having a SNR preserved at high resolution given a particular increase in effective area. If scale-invariance continues to prevail at smaller scales, the conclusion reached with SoHO/EIT images can be transposed

  5. The solar eruption of 13 May 2005: EISCAT and MERLIN observations of a coronal radio burst

    Directory of Open Access Journals (Sweden)

    R. A. Jones

    2006-09-01

    Full Text Available We report results from EISCAT and MERLIN observations of radio scintillation during a solar eruptive event in May 2005. Anomalous increases in signal strength detected at sites more than 2000 km apart are shown to arise from the detection of a strong coronal radio burst in the distant off-axis response of the MERLIN and EISCAT antennas. These observations show that EISCAT is capable of detecting the signatures of explosive events in the solar atmosphere with a high degree of time resolution. We further suggest that the highly time-structured variation in signal strength caused by distant off-axis detection of a powerful coronal radio signal could provide an explanation for previously unexplained anomalies in EISCAT IPS observations, as well as being a potential source of errors in active observations using radar codes with a completion time longer than the time-variation of the coronal signal.

  6. Prediction of coronal structure of the solar eclipse of October 23, 1976

    International Nuclear Information System (INIS)

    Schatten, K.H.

    1976-01-01

    Earlier work on the prediction of solar eclipse coronal structures is briefly summarised. A computer drawn plot made on October 18 1976 showed the field time structure predicted for the time of the solar eclipse on October 23. A very dipolar coronal field was indicated, and a very large equatorial streamer was predicted for both the east and west limbs of the Sun, due to the lack of very strong active regions near either limb. Nested coronal arches were seen within this equatorial streamer, and many small arches were also seen on both limbs. The main feature, however, is the prediction of the two large bright streamers marking the solar equator, with polar plumes in a characteristic dipole fashion. At the time of the eclipse it is hoped that a high resolution photograph will allow much of the structure to be discovered. (U.K.)

  7. Pictorial essay of ultrasound-reconstructed coronal plane images of the uterus in different uterine pathologies.

    Science.gov (United States)

    Grigore, Mihaela; Grigore, Anamaria; Gafitanu, Dumitru; Furnica, Cristina

    2018-04-01

    Imaging in the major planes (horizontal, coronal, and sagittal) of the uterus is important for determining anatomy and allowing the findings to be standardized, and for evaluating and diagnosing different pathological conditions in clinical practice. Examination of the coronal plane is an important step in identifying uterine pathologies and their relationships to the endometrial canal. Three-dimensional (3D) ultrasound reveals the normal anatomy better and improves the depiction of abnormal anatomy, as the coronal plane of the uterus can easily be obtained using 3D reconstruction techniques. Our pictorial essay demonstrates that adding 3D ultrasound to a routine gynecological workup can be beneficial for clinicians, enabling a precise diagnosis to be made. In addition, the volumes obtained and stored by 3D ultrasound can allow students or residents to become more familiar with normal and abnormal pelvic structures. Clin. Anat. 31:373-379, 2018. © 2017 Wiley Periodicals, Inc. © 2017 Wiley Periodicals, Inc.

  8. REDEFINING THE BOUNDARIES OF INTERPLANETARY CORONAL MASS EJECTIONS FROM OBSERVATIONS AT THE ECLIPTIC PLANE

    Energy Technology Data Exchange (ETDEWEB)

    Cid, C.; Palacios, J.; Saiz, E.; Guerrero, A. [Space Research Group—Space Weather, Departamento de Física y Matemáticas, Universidad de Alcalá, Alcalá de Henares (Spain)

    2016-09-01

    On 2015 January 6–7, an interplanetary coronal mass ejection (ICME) was observed at L1. This event, which can be associated with a weak and slow coronal mass ejection, allows us to discuss the differences between the boundaries of the magnetic cloud and the compositional boundaries. A fast stream from a solar coronal hole surrounding this ICME offers a unique opportunity to check the boundaries’ process definition and to explain differences between them. Using Wind and ACE data, we perform a complementary analysis involving compositional, magnetic, and kinematic observations providing relevant information regarding the evolution of the ICME as travelling away from the Sun. We propose erosion, at least at the front boundary of the ICME, as the main reason for the difference between the boundaries, and compositional signatures as the most precise diagnostic tool for the boundaries of ICMEs.

  9. Communicating with the coroner: how religion, culture, and family concerns may influence autopsy decision making.

    Science.gov (United States)

    Carpenter, Belinda; Adkins, Glenda; Barnes, Michael; Naylor, Charles; Begum, Nelufa

    2011-04-01

    Based on coronial data gathered in the state of Queensland in 2004, this article reviews how a change in legislation may have impacted autopsy decision making by coroners. More specifically, the authors evaluated whether the requirement that coronial autopsy orders specify the level of invasiveness of an autopsy to be performed by a pathologist was affected by the further requirement that coroners take into consideration a known religion, culture, and/or raised family concern before making such an order. Preliminary data reveal that the cultural status of the deceased did not affect coronial autopsy decision making. However, a known religion with a proscription against autopsy and a raised family concern appeared to be taken into account by coroners when making autopsy decisions and tended to decrease the invasiveness of the autopsy ordered from a full internal examination to either a partial internal examination or an external-only examination of the body. The impact of these findings is briefly discussed.

  10. Added value of using a CT coronal reformation to diagnose adnexal torsion

    Energy Technology Data Exchange (ETDEWEB)

    Jung, Sung Il; Park, Hee Sun; Yim, Young Hee; Jeon, Hae Jeong; Yu, Mi Hye; Kim, Young Jun [Dept. of Radiology, Konkuk University School of Medicine, Research Institute of Medical Science, Seoul (Korea, Republic of); Jeong, Kyung Ah [Dept. of Obstetrics and Gynecology, School of Medicine, Ewha Womans University, Seoul (Korea, Republic of)

    2015-08-15

    To evaluate the increased value of using coronal reformation of a transverse computed tomography (CT) scan for detecting adnexal torsion. This study included 106 woman suspected of having adnexal torsion who underwent CT with coronal reformations and subsequent surgical exploration. Two readers independently recorded the CT findings, such as the thickening of a fallopian tube, twisting of the adnexal pedicle, eccentric smooth wall thickening of the torsed adnexal mass, eccentric septal thickening of the torsed adnexal mass, eccentric poor enhancement of the torsed adnexal mass, uterine deviation to the twisted side, ascites or infiltration of pelvic fat, and the overall impression of adnexal torsion with a transverse scan alone or combined with coronal reformation and a transverse scan. The areas under the receiver operating characteristic curves (AUCs), sensitivity, specificity, and positive predictive value were used to compare diagnostic performance. Fifty-two patients were confirmed to have adnexal torsion. The addition of coronal reformations to the transverse scan improved AUCs for readers 1 and 2 from 0.74 and 0.75 to 0.92 and 0.87, respectively, for detecting adnexal torsion (p < 0.001 and p = 0.004, respectively). Sensitivity of CT for detecting twisting of the adnexal pedicle increased significantly for readers 1 and 2 from 0.27 and 0.29 with a transverse scan alone to 0.79 and 0.77 with a combined coronal reformation and a transverse scan, respectively (p < 0.001 and p < 0.001, respectively). Use of a coronal reformation with transverse CT images improves detection of adnexal torsion.

  11. CORONAL AND CHROMOSPHERIC SIGNATURES OF LARGE-SCALE DISTURBANCES ASSOCIATED WITH A MAJOR SOLAR ERUPTION

    Energy Technology Data Exchange (ETDEWEB)

    Zong, Weiguo [Key Laboratory of Space Weather, National Center for Space Weather, China Meteorological Administration, Beijing 100081 (China); Dai, Yu, E-mail: ydai@nju.edu.cn [Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210023 (China)

    2015-08-20

    We present both coronal and chromospheric observations of large-scale disturbances associated with a major solar eruption on 2005 September 7. In the Geostationary Operational Environmental Satellites/Solar X-ray Imager (SXI), arclike coronal brightenings are recorded propagating in the southern hemisphere. The SXI front shows an initially constant speed of 730 km s{sup −1} and decelerates later on, and its center is near the central position angle of the associated coronal mass ejection (CME) but away from the flare site. Chromospheric signatures of the disturbances are observed in both Mauna Loa Solar Observatory (MLSO)/Polarimeter for Inner Coronal Studies Hα and MLSO/Chromospheric Helium I Imaging Photometer He i λ10830 and can be divided into two parts. The southern signatures occur in regions where the SXI front sweeps over, with the Hα bright front coincident with the SXI front, while the He i dark front lags the SXI front but shows a similar kinematics. Ahead of the path of the southern signatures, oscillations of a filament are observed. The northern signatures occur near the equator, with the Hα and He i fronts coincident with each other. They first propagate westward and then deflect to the north at the boundary of an equatorial coronal hole. Based on these observational facts, we suggest that the global disturbances are associated with the CME lift-off and show a hybrid nature: a mainly non-wave CME flank nature for the SXI signatures and the corresponding southern chromospheric signatures, and a shocked fast-mode coronal MHD wave nature for the northern chromospheric signatures.

  12. Dynamics of low density coronal plasma in low current x-pinches

    International Nuclear Information System (INIS)

    Haas, D; Bott, S C; Vikhrev, V; Eshaq, Y; Ueda, U; Zhang, T; Baranova, E; Krasheninnikov, S I; Beg, F N

    2007-01-01

    Experiments were performed on an x-pinch using a pulsed power current generator capable of producing an 80 kA current with a rise time of 50 ns. Molybdenum wires with and without gold coating were employed to study the effect of high z coating on the low-density ( 18 cm -3 ) coronal plasma dynamics. A comparison of images from XUV frames and optical probing shows that the low density coronal plasma from the wires initially converges at the mid-plane immediately above and below the cross-point. A central jet is formed which moves with a velocity of 6 x 10 4 ms -1 towards both electrodes forming a z-pinch column before the current maximum. A marked change in the low density coronal plasma dynamics was observed when molybdenum wires coated with ∼ 0.09 μm of gold were used. The processes forming the jet structure were delayed relative to bare Mo x-pinches, and the time-resolved x-ray emission also showed differences. An m = 0 instability was observed in the coronal plasma along the x-pinch legs, which were consistent with x-ray PIN diode signals in which x-ray pulses were observed before x-ray spot formation. These early time x-ray pulses were not observed with pure molybdenum x-pinches. These observations indicate that a thin layer of gold coating significantly changes the coronal plasma behaviour. Two dimensional MHD simulations were performed and qualitatively agree with experimental observations of low density coronal plasma

  13. RECONNECTION-DRIVEN CORONAL-HOLE JETS WITH GRAVITY AND SOLAR WIND

    Energy Technology Data Exchange (ETDEWEB)

    Karpen, J. T.; DeVore, C. R.; Antiochos, S. K. [Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt MD 20771 (United States); Pariat, E. [LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, F-92195 Meudon (France)

    2017-01-01

    Coronal-hole jets occur ubiquitously in the Sun's coronal holes, at EUV and X-ray bright points associated with intrusions of minority magnetic polarity. The embedded-bipole model for these jets posits that they are driven by explosive, fast reconnection between the stressed closed field of the embedded bipole and the open field of the surrounding coronal hole. Previous numerical studies in Cartesian geometry, assuming uniform ambient magnetic field and plasma while neglecting gravity and solar wind, demonstrated that the model is robust and can produce jet-like events in simple configurations. We have extended these investigations by including spherical geometry, gravity, and solar wind in a nonuniform, coronal hole-like ambient atmosphere. Our simulations confirm that the jet is initiated by the onset of a kink-like instability of the internal closed field, which induces a burst of reconnection between the closed and external open field, launching a helical jet. Our new results demonstrate that the jet propagation is sustained through the outer corona, in the form of a traveling nonlinear Alfvén wave front trailed by slower-moving plasma density enhancements that are compressed and accelerated by the wave. This finding agrees well with observations of white-light coronal-hole jets, and can explain microstreams and torsional Alfvén waves detected in situ in the solar wind. We also use our numerical results to deduce scaling relationships between properties of the coronal source region and the characteristics of the resulting jet, which can be tested against observations.

  14. How can we ensure that the coroner's autopsy is not an invasion of human rights?

    Science.gov (United States)

    Leadbeatter, Stephen; James, Ryk

    2018-01-01

    Despite public inquiries, and some changes to legislation following high-profile multiple homicides that were not detected by autopsy, coroners continue to rely largely on the autopsy. Regardless of the extent of quality failings and excess deaths at some hospitals, not detected through the coroner system, the autopsy is scarcely used by hospitals to monitor standards and educate. To explore when a compulsory medicolegal autopsy should, and should not, be used. Two hundred and thirty-six cases referred to a senior coroner were evaluated by pathologists with long experience of forensic, coronial and hospital autopsies, using detailed antecedent medical and circumstantial information: after their advice, the senior coroner decided what kind of autopsy provided sufficient information for his purposes. In nearly 40% (n=88) of deaths where the senior coroner accepted jurisdiction, issues raised could be resolved through analysis of medical records and antecedent information, supplemented only by detailed external examination of the body. Timely provision of sufficient information allows informed decisions about the requirement for, and nature and extent of, medical investigations into a death: unnecessary post mortem dissection is avoided, protecting the rights, under Articles 8 and 9 of the Human Rights Act 1998, of the bereaved to privacy, family life and religious practice. Although improvements in healthcare can undoubtedly result from detailed coroners' inquiries, those deaths where the matters investigated relate only to the accuracy of a natural cause of death or sit with a healthcare provider's internal quality assurance, should be investigated by the healthcare system in collaboration with the bereaved. © Article author(s) (or their employer(s) unless otherwise stated in the text of the article) 2018. All rights reserved. No commercial use is permitted unless otherwise expressly granted.

  15. CORONAL AND CHROMOSPHERIC SIGNATURES OF LARGE-SCALE DISTURBANCES ASSOCIATED WITH A MAJOR SOLAR ERUPTION

    International Nuclear Information System (INIS)

    Zong, Weiguo; Dai, Yu

    2015-01-01

    We present both coronal and chromospheric observations of large-scale disturbances associated with a major solar eruption on 2005 September 7. In the Geostationary Operational Environmental Satellites/Solar X-ray Imager (SXI), arclike coronal brightenings are recorded propagating in the southern hemisphere. The SXI front shows an initially constant speed of 730 km s −1 and decelerates later on, and its center is near the central position angle of the associated coronal mass ejection (CME) but away from the flare site. Chromospheric signatures of the disturbances are observed in both Mauna Loa Solar Observatory (MLSO)/Polarimeter for Inner Coronal Studies Hα and MLSO/Chromospheric Helium I Imaging Photometer He i λ10830 and can be divided into two parts. The southern signatures occur in regions where the SXI front sweeps over, with the Hα bright front coincident with the SXI front, while the He i dark front lags the SXI front but shows a similar kinematics. Ahead of the path of the southern signatures, oscillations of a filament are observed. The northern signatures occur near the equator, with the Hα and He i fronts coincident with each other. They first propagate westward and then deflect to the north at the boundary of an equatorial coronal hole. Based on these observational facts, we suggest that the global disturbances are associated with the CME lift-off and show a hybrid nature: a mainly non-wave CME flank nature for the SXI signatures and the corresponding southern chromospheric signatures, and a shocked fast-mode coronal MHD wave nature for the northern chromospheric signatures

  16. The Coronal Analysis of SHocks and Waves (CASHeW) framework

    Science.gov (United States)

    Kozarev, Kamen A.; Davey, Alisdair; Kendrick, Alexander; Hammer, Michael; Keith, Celeste

    2017-11-01

    Coronal bright fronts (CBF) are large-scale wavelike disturbances in the solar corona, related to solar eruptions. They are observed (mostly in extreme ultraviolet (EUV) light) as transient bright fronts of finite width, propagating away from the eruption source location. Recent studies of individual solar eruptive events have used EUV observations of CBFs and metric radio type II burst observations to show the intimate connection between waves in the low corona and coronal mass ejection (CME)-driven shocks. EUV imaging with the atmospheric imaging assembly instrument on the solar dynamics observatory has proven particularly useful for detecting large-scale short-lived CBFs, which, combined with radio and in situ observations, holds great promise for early CME-driven shock characterization capability. This characterization can further be automated, and related to models of particle acceleration to produce estimates of particle fluxes in the corona and in the near Earth environment early in events. We present a framework for the coronal analysis of shocks and waves (CASHeW). It combines analysis of NASA Heliophysics System Observatory data products and relevant data-driven models, into an automated system for the characterization of off-limb coronal waves and shocks and the evaluation of their capability to accelerate solar energetic particles (SEPs). The system utilizes EUV observations and models written in the interactive data language. In addition, it leverages analysis tools from the SolarSoft package of libraries, as well as third party libraries. We have tested the CASHeW framework on a representative list of coronal bright front events. Here we present its features, as well as initial results. With this framework, we hope to contribute to the overall understanding of coronal shock waves, their importance for energetic particle acceleration, as well as to the better ability to forecast SEP events fluxes.

  17. Magnetic Untwisting in Jets that Go into the Outer Solar Corona in Polar Coronal Holes

    Science.gov (United States)

    Moore, Ronald L.; Sterling, Alphonse C.; Falconer, David

    2014-06-01

    We present results from a study of 14 jets that were observed in SDO/AIA EUV movies to erupt in the Sun’s polar coronal holes. These jets were similar to the many other jets that erupt in coronal holes, but reached higher than the vast majority, high enough to be observed in the outer corona beyond 2 solar radii from Sun center by the SOHO/LASCO/C2 coronagraph. We illustrate the characteristic structure and motion of these high-reaching jets by showing observations of two representative jets. We find that (1) the speed of the jet front from the base of the corona out to 2-3 solar radii is typically several times the sound speed in jets in coronal holes, (2) each high-reaching jet displays unusually large rotation about its axis (spin) as it erupts, and (3) in the outer corona, many jets display lateral swaying and bending of the jet axis with an amplitude of a few degrees and a period of order 1 hour. From these observations we infer that these jets are magnetically driven, propose that the driver is a magnetic-untwisting wave that is basically a large-amplitude (non-linear) torsional Alfven wave that is put into the open magnetic field in the jet by interchange reconnection as the jet erupts, and estimate that the magnetic-untwisting wave loses most of its energy before reaching the outer corona. These observations of high-reaching coronal jets suggest that the torsional magnetic waves observed in Type-II spicules can similarly dissipate in the corona and thereby power much of the coronal heating in coronal holes and quiet regions. This work is funded by the NASA/SMD Heliophysics Division’s Living With a Star Targeted Research & Technology Program.

  18. The angle of inclination of the native ACL in the coronal and sagittal planes.

    Science.gov (United States)

    Reid, Jonathan C; Yonke, Bret; Tompkins, Marc

    2017-04-01

    The purpose of this cross-sectional study was to evaluate the angle of inclination of the native anterior cruciate ligament (ACL) in both the sagittal and coronal planes and to evaluate these findings based on sex, height, BMI, and skeletal maturity. Inclusion criteria for the study included patients undergoing routine magnetic resonance imaging (MRI) of the knee at a single outpatient orthopedic center who had an intact ACL on MRI. Measurements of the angle of inclination were made on MRIs in both the sagittal and coronal planes. Patients were compared based on sex, height, BMI, and skeletal maturity. One-hundred and eighty-eight patients were included (36 skeletally immature/152 skeletally mature; 98 male/90 female). The overall angle of inclination was 74.3° ± 4.8° in the coronal plane and 46.9° ± 4.9° in the sagittal plane. Skeletally immature patients (coronal: 71.8° ± 6.1°; sagittal: 44.7° ± 5.5°) were significantly different in both coronal and sagittal planes (P = 0.04 and 0.01, respectively) from skeletally mature patients (coronal: 75.3° ± 4.7°; sagittal: 47.4° ± 4.7°). There were no differences based on sex, height, or BMI. There are differences between the angle of inclination findings in this study and other studies, which could be due to MRI and measurement techniques. Clinically, skeletal maturity may be important to account for when using the ACL angle of inclination to evaluate anatomic ACL reconstruction. Prognostic retrospective study, Level of evidence III.

  19. Coronal mass ejections, interplanetary shocks in relation with forbush decreases associated with intense geomagnetic storms

    International Nuclear Information System (INIS)

    Verma, P L; Patel, Nand Kumar; Prajapati, Mateswari

    2014-01-01

    Coronal mass ejections (CMEs} are the most energetic solar events in which large amount of solar plasma materials are ejected from the sun into heliosphere, causing major disturbances in solar wind plasma, Interplanetary shocks, Forbush decrease(Fds) in cosmic ray intensity and geomagnetic storms. We have studied Forbush decreases associated with intense geomagnetic storms observed at Oulu super neutron monitor, during the period of May 1998-Dec 2006 with coronal mass ejections (CMEs), X-ray solar flares and interplanetary shocks. We have found that all the (100%) Forbush decreases associated with intense geomagnetic storms are associated with halo and partial halo coronal mass ejections (CMEs). The association rate between halo and partial halo coronal mass ejections are found 96.00%and 04.00% respectively. Most of the Forbush decreases associated with intense geomagnetic storms (96.29%) are associated with X-ray solar flares of different categories . The association rates for X-Class, M-Class, and C- Class X -ray solar flares are found 34.62%, 50.00% and 15.38% respectively .Further we have concluded that majority of the Forbush decrease associated with intense geomagnetic storms are related to interplanetary shocks (92.30 %) and the related shocks are forward shocks. We have found positive co-relation with co-relation co-efficient .7025 between magnitudes of Forbush decreases associated with intense geomagnetic storms and speed of associated coronal mass ejections. Positive co-relation with co-relation co-efficient 0.48 has also been found between magnitudes of intense geomagnetic storms and speed of associated coronal mass ejections.

  20. Interactions of Dust Grains with Coronal Mass Ejections and Solar Cycle Variations of the F-Coronal Brightness

    Science.gov (United States)

    Ragot, B. R.; Kahler, S. W.

    2003-01-01

    The density of interplanetary dust increases sunward to reach its maximum in the F corona, where its scattered white-light emission dominates that of the electron K corona above about 3 Solar Radius. The dust will interact with both the particles and fields of antisunward propagating coronal mass ejections (CMEs). To understand the effects of the CME/dust interactions we consider the dominant forces, with and without CMEs. acting on the dust in the 3-5 Solar Radius region. Dust grain orbits are then computed to compare the drift rates from 5 to 3 Solar Radius. for periods of minimum and maximum solar activity, where a simple CME model is adopted to distinguish between the two periods. The ion-drag force, even in the quiet solar wind, reduces the drift time by a significant factor from its value estimated with the Poynting-Robertson drag force alone. The ion-drag effects of CMEs result in even shorter drift times of the large (greater than or approx. 3 microns) dust grains. hence faster depletion rates and lower dust-pain densities, at solar maxima. If dominated by thermal emission, the near-infrared brightness will thus display solar cycle variations close to the dust plane of symmetry. While trapping the smallest of the grains, the CME magnetic fields also scatter the grains of intermediate size (0.1-3 microns) in latitude. If light scattering by small grains close to the Sun dominates the optical brightness. the scattering by the CME magnetic fields will result in a solar cycle variation of the optical brightness distribution not exceeding 100% at high latitudes, with a higher isotropy reached at solar maxima. A good degree of latitudinal isotropy is already reached at low solar activity since the magnetic fields of the quiet solar wind so close to the Sun are able to scatter the small (less than or approx. 3 microns) grains up to the polar regions in only a few days or less, producing strong perturbations of their trajectories in less than half their orbital

  1. Normal anatomy of the female pelvis in axial, coronal, and sagittal planes demonstrated with reformatted CT

    International Nuclear Information System (INIS)

    Constant, O.C.; Cooke, J.C.; Parsons, C.A.

    1987-01-01

    Axial CT is used in assessing gynecologic malignancies. Accurate delineation of local tumor extent in carcinoma of the cervix is important in initial staging and in planning subsequent management. A modified scanning technique produces reformatted coronal and sagittal images, which demonstrate additional valuable information about the cardinal ligaments, parametria, ureters, boundaries between the cervix, bladder, and rectum, and extension to vagina and uterus. This information is illustrated by representative axial, coronal, and sagittal scans. Familiarity with normal appearances is essential to allow correct interpretation of pathology

  2. Energy dissipation of Alfven wave packets deformed by irregular magnetic fields in solar-coronal arches

    Science.gov (United States)

    Similon, Philippe L.; Sudan, R. N.

    1989-01-01

    The importance of field line geometry for shear Alfven wave dissipation in coronal arches is demonstrated. An eikonal formulation makes it possible to account for the complicated magnetic geometry typical in coronal loops. An interpretation of Alfven wave resonance is given in terms of gradient steepening, and dissipation efficiencies are studied for two configurations: the well-known slab model with a straight magnetic field, and a new model with stochastic field lines. It is shown that a large fraction of the Alfven wave energy flux can be effectively dissipated in the corona.

  3. Required Critical Conversations Between Medical Examiners/Coroners and Forensic Nurses.

    Science.gov (United States)

    Infanti Mraz, Megan A

    2016-01-01

    Forensic teams work with the deceased and their families on a daily basis. The forensic team fulfills an important role during the death process and serves as a medium between the medical community and investigative community. The medical examiner, or coroner, depending on jurisdiction, plays a critical role in the death investigation, whose assessments and findings are a key element in care for the deceased in relation to the investigation. Communication regarding care for the deceased is critical to the completion of the investigation. Nine key discussion points are addressed as a means to launch communications between the forensic team and the medical examiner/coroner's office.

  4. Casos de Estudio de Distribuciones de Probabilidad para Turismo

    OpenAIRE

    Fernández Morales, Antonio

    2016-01-01

    Este trabajo propone diversos casos de estudio para el estudio de las distribuciones de probabilidad aplicadas a la investigación y la práctica profesional en el ámbito del turismo. Se afronta el estudio de distribuciones de probabilidad, tanto de variables aleatorias discretas como continuas.

  5. 77 FR 31041 - Draft Standards and Best Practices for Interaction Between Medical Examiner/Coroner and Organ and...

    Science.gov (United States)

    2012-05-24

    ... Best Practices for Interaction Between Medical Examiner/Coroner and Organ and Tissue Procurement... titled ``Organ and Tissue Procurement Committee Standards and Best Practices for Interaction Between Medical Examiner/Coroner Offices and Organ Tissue Procurement Organizations'' from May 12, 2012, to June...

  6. A long look at MCG-5-23-16 with NuSTAR. I. relativistic reflection and coronal properties

    DEFF Research Database (Denmark)

    Zoghbi, Abderahmen; Matt, G; Miller, J. M.

    2017-01-01

    between the cutoff energy and both the hard X-ray flux and spectral index. The measurements imply that the coronal plasma is not at the runaway electron-positron pair limit, and instead contains mostly electrons. The observed variability in the coronal properties is driven by a variable optical depth...

  7. H and K (Ca II) emissions as observed in coronal spectrum in the July 20, 1963 solar eclipse

    International Nuclear Information System (INIS)

    Cavallini, F.; Righini, A.

    1975-01-01

    From a detailed analysis of a coronal spectrum taken from a DC-8 jet airplane during the Eclipse of 20 July, 1963 a rough model of a coronal cold region (T approximately 10 5 K) has been obtained. The model explains the presence of the abnormal H and K (Ca II) emissions and the large amount of F corona present in the spectrum. (Auth.)

  8. Estudios de competitividad en sistemas urbano - territoriales

    Directory of Open Access Journals (Sweden)

    Esteban Soms García

    2007-05-01

    El Ministerio de Planificación y Cooperación de Chile, ha desarrollado varios estudios relacionados con la competitividad regional, destinados a pronosticar y evaluar los impactos positivos y negativos que podrían derivarse de los recientes Acuerdos de Libre Comercio suscritos por Chile con la Comunidad Europea, Estados Unidos y Corea, más los acuerdos ad portas con los Países de la APEC. En lo referente a competitividad urbana, destacan algunos estudios y proyectos relacionados con el programa gubernamental "Ciudades para el Bicentenario", impulsado el Ministerio de Vivienda y Urbanismo y los Gobiernos Regionales de Antofagasta, Bio Bio, Valparaíso y Santiago.

  9. Estrategia organizacional: una propuesta de estudio

    Directory of Open Access Journals (Sweden)

    Ángela Lucía Noguera Hidalgo

    2014-01-01

    Full Text Available El concepto de estrategia en el contexto de las organizaciones empresariales es uno de los temas que genera gran interés en los asuntos del management. Sin embargo, la proposición de nuevos enfoques no ha aportado significativamente al avance en el estudio de este concepto. El estancamiento se hace evidente, razón por la cual el presente documento esboza una propuesta que reúne algunos de los retos para el estudio de la estrategia. En él se presenta una revisión que deja por sentados los posibles caminos a seguir, los cuales contribuyen a la perdurabilidad de las organizaciones.

  10. ESTUDIOS (INTERCULTURALES EN CLAVE DE-COLONIAL

    Directory of Open Access Journals (Sweden)

    Catherine Walsh

    2010-01-01

    Full Text Available Los «estudios culturales» en América Latina forman parte de una política de nombrar inscrita en legados y cartografiados frecuentemente como totalidad, ocultando o dejando pasar por alto las diferencias a su interior. Este articula examina desde dónde nacen los estudios culturales en América Latina en general y en la Universidad Andina Simón Bolívar en Quito en particular, con qué política de nombramiento, qué proyecto(s y qué bases y perspectivas de conocimiento. Considera qué implica concebir y construir los estudios culturales como proyecto político-intelectual, inter-cultural, inter-epistémico y de orientación de-colonial y los desafíos y obstáculos al respecto, incluyendo dentro de la problemática misma de la «uni»-versidad.

  11. Coronal reconstruction of unenhanced abdominal CT for correct ureteral stone size classification

    Energy Technology Data Exchange (ETDEWEB)

    Berkovitz, Nadav; Simanovsky, Natalia; Hiller, Nurith [Hadassah Mount Scopus - Hebrew University Medical Center, Department of Radiology, Jerusalem (Israel); Katz, Ran [Hadassah Mount Scopus - Hebrew University Medical Center, Department of Urology, Jerusalem (Israel); Salama, Shaden [Hadassah Mount Scopus - Hebrew University Medical Center, Department of Emergency Medicine, Jerusalem (Israel)

    2010-05-15

    To determine whether size measurement of a urinary calculus in coronal reconstruction of computed tomography (CT) differs from stone size measured in the axial plane, and whether the difference alters clinical decision making. We retrospectively reviewed unenhanced CT examinations of 150 patients admitted to the emergency room (ER) with acute renal colic. Maximal ureteral calculus size was measured on axial slices and coronal reconstructions. Clinical significance was defined as an upgrading or downgrading of stone size according to accepted thresholds of treatment: {<=}5 mm, 6-9 mm and {>=}10 mm. There were 151 stones in 150 patients (male:female 115:34, mean age 41 years). Transverse stone diameters ranged from 1 to 11 mm (mean 4 mm). On coronal images, 56 (37%) stones were upgraded in severity; 46 (30%) from below 5 mm to 6 mm or more, and ten (7%) from 6-9 mm to 10 mm or more. Transverse measurement on the axial slices enabled correct categorization of 95 stones (63%). Transverse calculus measurement on axial slices often underestimates stone size and provides incorrect clinical classification of the true maximal stone diameter. Coronal reconstruction provides additional information in patients with renal colic that may alter treatment strategy. (orig.)

  12. Coronal reconstruction of unenhanced abdominal CT for correct ureteral stone size classification

    International Nuclear Information System (INIS)

    Berkovitz, Nadav; Simanovsky, Natalia; Hiller, Nurith; Katz, Ran; Salama, Shaden

    2010-01-01

    To determine whether size measurement of a urinary calculus in coronal reconstruction of computed tomography (CT) differs from stone size measured in the axial plane, and whether the difference alters clinical decision making. We retrospectively reviewed unenhanced CT examinations of 150 patients admitted to the emergency room (ER) with acute renal colic. Maximal ureteral calculus size was measured on axial slices and coronal reconstructions. Clinical significance was defined as an upgrading or downgrading of stone size according to accepted thresholds of treatment: ≤5 mm, 6-9 mm and ≥10 mm. There were 151 stones in 150 patients (male:female 115:34, mean age 41 years). Transverse stone diameters ranged from 1 to 11 mm (mean 4 mm). On coronal images, 56 (37%) stones were upgraded in severity; 46 (30%) from below 5 mm to 6 mm or more, and ten (7%) from 6-9 mm to 10 mm or more. Transverse measurement on the axial slices enabled correct categorization of 95 stones (63%). Transverse calculus measurement on axial slices often underestimates stone size and provides incorrect clinical classification of the true maximal stone diameter. Coronal reconstruction provides additional information in patients with renal colic that may alter treatment strategy. (orig.)

  13. Anatomy-Based navigation for ventriculostomy: Nasion-coronal suture distance measurement

    Directory of Open Access Journals (Sweden)

    Mevci Özdemir

    2014-09-01

    Full Text Available Objective: In this study we aimed to determine a landmark that can be measured through the skin with nasal mid-point (bregma to coronal suture, and additionally an average value was calculated. We report, to our knowledge, the distance between the nasion-coronal sutures is reported for the first time in Turkish population. Methods: The study included 30 craniums and 30 frontal bones. Each skull from midline nasal suture to coronal suture curved up at the distance was measured with tape measure. Results: Mean values were determined. Nasal suture between coronal suture distance average 12,2 cm (min10,3 cm, up to 13,5 cm were detected. Conclusion: Nasal suture is an easily palpable area through the skin. A small incision is carried down through skin to bone at the spot 12 cm back from the nasion 3 cm lateral to the midline for ventricular drainage operation. This data provide practical information for neurosurgeon and is available everywhere. J Clin Exp Invest 2014; 5 (3: 368-370

  14. CORONAL MASS EJECTIONS AS A MECHANISM FOR PRODUCING IR VARIABILITY IN DEBRIS DISKS

    International Nuclear Information System (INIS)

    Osten, Rachel; Livio, Mario; Lubow, Steve; Pringle, J. E.; Soderblom, David; Valenti, Jeff

    2013-01-01

    Motivated by recent observations of short-timescale variations in the infrared emission of circumstellar disks, we propose that coronal mass ejections can remove dust grains on timescales as short as a few days. Continuous monitoring of stellar activity, coupled with infrared observations, can place meaningful constraints on the proposed mechanism.

  15. Improvements on coronal hole detection in SDO/AIA images using supervised classification

    Directory of Open Access Journals (Sweden)

    Reiss Martin A.

    2015-01-01

    Full Text Available We demonstrate the use of machine learning algorithms in combination with segmentation techniques in order to distinguish coronal holes and filaments in SDO/AIA EUV images of the Sun. Based on two coronal hole detection techniques (intensity-based thresholding, SPoCA, we prepared datasets of manually labeled coronal hole and filament channel regions present on the Sun during the time range 2011–2013. By mapping the extracted regions from EUV observations onto HMI line-of-sight magnetograms we also include their magnetic characteristics. We computed shape measures from the segmented binary maps as well as first order and second order texture statistics from the segmented regions in the EUV images and magnetograms. These attributes were used for data mining investigations to identify the most performant rule to differentiate between coronal holes and filament channels. We applied several classifiers, namely Support Vector Machine (SVM, Linear Support Vector Machine, Decision Tree, and Random Forest, and found that all classification rules achieve good results in general, with linear SVM providing the best performances (with a true skill statistic of ≈ 0.90. Additional information from magnetic field data systematically improves the performance across all four classifiers for the SPoCA detection. Since the calculation is inexpensive in computing time, this approach is well suited for applications on real-time data. This study demonstrates how a machine learning approach may help improve upon an unsupervised feature extraction method.

  16. Use of limited MR protocol (coronal STIR) in the evaluation of patients with hip pain

    International Nuclear Information System (INIS)

    Khoury, N.J.; Birjawi, G.A.; Hourani, M.H.; Chaaya, M.

    2003-01-01

    To assess the role of a limited MR protocol (coronal STIR) as the initial part of the MR examination in patients with hip pain. Eighty-five patients presenting with hip pain, and normal radiographs of the pelvis, and who underwent our full MR protocol for hips were included retrospectively in the study. The full protocol consists of coronal T1-weighted and short tau inversion-recovery (STIR), and axial T2-weighted sequences. Ninety-three MR examinations were performed. Two radiologists interpreted the STIR (limited) examinations and the full studies separately, masked to each other's findings and to the final diagnosis. Comparison between the two protocols was then undertaken. For both readers, all normal MR examinations on the coronal STIR limited protocol were normal on the full protocol, with an interobserver reliability of 0.96. The STIR protocol was able to detect the presence or absence of an abnormality in 100% of cases (sensitivity). The STIR-only protocol provided a specific diagnosis in only 65% of cases (specificity). A normal coronal STIR study of the hips in patients with hip pain and normal radiographs precludes the need for further pelvic MR sequences. Any abnormality detected on this limited protocol should be further assessed by additional MR sequences. (orig.)

  17. The classification of ambiguity in polarimetric reconstruction of coronal mass ejection

    International Nuclear Information System (INIS)

    Dai, Xinghua; Wang, Huaning; Huang, Xin; Du, Zhanle; He, Han

    2014-01-01

    The Thomson scattering theory indicates that there exist explicit and implicit ambiguities in polarimetric analyses of coronal mass ejection (CME) observations. We suggest a classification for these ambiguities in CME reconstruction. Three samples, including double explicit, mixed, and double implicit ambiguity, are shown with the polarimetric analyses of STEREO CME observations. These samples demonstrate that this classification is helpful for improving polarimetric reconstruction.

  18. Automatic recognition of coronal type II radio bursts: The ARBIS 2 method and first observations

    Science.gov (United States)

    Lobzin, Vasili; Cairns, Iver; Robinson, Peter; Steward, Graham; Patterson, Garth

    Major space weather events such as solar flares and coronal mass ejections are usually accompa-nied by solar radio bursts, which can potentially be used for real-time space weather forecasts. Type II radio bursts are produced near the local plasma frequency and its harmonic by fast electrons accelerated by a shock wave moving through the corona and solar wind with a typi-cal speed of 1000 km s-1 . The coronal bursts have dynamic spectra with frequency gradually falling with time and durations of several minutes. We present a new method developed to de-tect type II coronal radio bursts automatically and describe its implementation in an extended Automated Radio Burst Identification System (ARBIS 2). Preliminary tests of the method with spectra obtained in 2002 show that the performance of the current implementation is quite high, ˜ 80%, while the probability of false positives is reasonably low, with one false positive per 100-200 hr for high solar activity and less than one false event per 10000 hr for low solar activity periods. The first automatically detected coronal type II radio bursts are also presented. ARBIS 2 is now operational with IPS Radio and Space Services, providing email alerts and event lists internationally.

  19. The Role of the Coroner in School Bus Accident Prevention: Some Recommendations.

    Science.gov (United States)

    Fox, Michael

    1995-01-01

    Following the deaths of two elementary school students in bus-related accidents in 1992, the Coroner of Quebec held extensive hearings investigating school bus safety and accident prevention. A subsequent report addressed responsibilities of government and school board officials to correct deficiencies in school bus services and provided…

  20. Study on the usefulness of whole body SPECT coronal image, MIP image in 67Ga scintigraphy

    International Nuclear Information System (INIS)

    Kawamura, Seiji

    2002-01-01

    In this study, we examined the usefulness of whole body coronal images and whole body cine display MIP images (CMIP) upon which image processing was carried out after whole body SPECT in comparison to the usefulness of whole body images (WB/SC) compensated by scattered radiation in tumor/inflammation scintigraphy with 67 Ga-citrate ( 67 Ga). Image interpretation was performed for the 120 patients with confirmed diagnoses, and the accuracy of their diagnoses was studied by three nuclear medical physicians and two clinical radiological technologists by means of sensitivity, specificity and ROC analysis. The resultant data show that sensitivity, specificity, accuracy and the area under the ROC curve Az in the WB/SC were approximately 65%, 86%, 74% and 0.724, respectively, whereas sensitivity, specificity, accuracy and Az of the image reading system in which CMIP is combined with whole body coronal images reconstructed by the OS-EM method were approximately 93%, 95%, 94% and 0.860, respectively. Furthermore, coronal images reconstructed by the OS-EM method tended to be superior to those produced by the FBP method in both diagnostic accuracy and ROC analysis. In conclusion, the image reading system in which CMIP is combined with whole body coronal images reconstructed by the OS-EM method was shown to be superior in diagnostic accuracy and ROC analysis. Our data suggest that whole body SPECT is an excellent technique as an alternative to WB/SC. (author)

  1. Tooth coronal index: Key for age estimation on digital panoramic radiographs

    Directory of Open Access Journals (Sweden)

    Ravleen Nagi

    2018-01-01

    Full Text Available Background: Assessment of age through teeth is one of the most reliable and simple method than skeletal remains, to calculate age of an individual. Objectives: The study was carried out with an aim to evaluate reliability of dental age assessment through tooth coronal index (TCI method. Materials and Methods: The digital panoramic radiographs of 100 subjects of Chhattisgarh aged 20–70 years were selected for the study. The measurements were performed on the JPEG images of selected panoramic radiographs by using Adobe Acrobat 7.0 professional software. The height of the crown, i.e., coronal height, and the height of the coronal pulp cavity, i.e., coronal pulp cavity height, of mandibular second premolars and first molars were measured in millimeter (mm and then TCI was calculated for each tooth. Actual age of a subject was compared with TCI of tooth and the acquired data were subjected to Pearson's correlation and unpaired t-tests. Results: Negative correlation was observed between the real age and TCI of mandibular first molar (r = −0.092, P = 0.365 and second premolar (r = −0.168, P = 0.096. Statistically significant difference was observed between real age and TCI for mandibular second premolar and first molar (P = 0.000 by unpaired t-test. Conclusion: TCI has the potential to estimate age of an individual on dental radiographs. It is simple, cost effective than histological methods and can be applied to both living and unknown dead.

  2. Solar coronal non-thermal processes (Solar Maximum Mission). Final report

    International Nuclear Information System (INIS)

    Hudson, H.S.

    1983-02-01

    The Solar Maximum Mission was used to study solar coronal phenomena in hard X-radiation, since its instrument complement included the first solar hard X-ray telescope. Phenomena related to those discovered from OSO-5 and OSO-7 observations were emphasized

  3. CORONAL DENSITY STRUCTURE AND ITS ROLE IN WAVE DAMPING IN LOOPS

    Energy Technology Data Exchange (ETDEWEB)

    Cargill, P. J. [Space and Atmospheric Physics, The Blackett Laboratory, Imperial College, London SW7 2BW (United Kingdom); De Moortel, I.; Kiddie, G., E-mail: p.cargill@imperial.ac.uk [School of Mathematics and Statistics, University of St Andrews, St Andrews, Scotland KY16 9SS (United Kingdom)

    2016-05-20

    It has long been established that gradients in the Alfvén speed, and in particular the plasma density, are an essential part of the damping of waves in the magnetically closed solar corona by mechanisms such as resonant absorption and phase mixing. While models of wave damping often assume a fixed density gradient, in this paper the self-consistency of such calculations is assessed by examining the temporal evolution of the coronal density. It is shown conceptually that for some coronal structures, density gradients can evolve in a way that the wave-damping processes are inhibited. For the case of phase mixing we argue that (a) wave heating cannot sustain the assumed density structure and (b) inclusion of feedback of the heating on the density gradient can lead to a highly structured density, although on long timescales. In addition, transport coefficients well in excess of classical are required to maintain the observed coronal density. Hence, the heating of closed coronal structures by global oscillations may face problems arising from the assumption of a fixed density gradient, and the rapid damping of oscillations may have to be accompanied by a separate (non-wave-based) heating mechanism to sustain the required density structuring.

  4. Communicating with the Coroner: How Religion, Culture, and Family Concerns May Influence Autopsy Decision Making

    Science.gov (United States)

    Carpenter, Belinda; Tait, Gordon; Adkins, Glenda; Barnes, Michael; Naylor, Charles; Begum, Nelufa

    2011-01-01

    Based on coronial data gathered in the state of Queensland in 2004, this article reviews how a change in legislation may have impacted autopsy decision making by coroners. More specifically, the authors evaluated whether the requirement that coronial autopsy orders specify the level of invasiveness of an autopsy to be performed by a pathologist…

  5. MINI-FILAMENT ERUPTION AS THE INITIATION OF A JET ALONG CORONAL LOOPS

    International Nuclear Information System (INIS)

    Hong, Junchao; Jiang, Yunchun; Yang, Jiayan; Yang, Bo; Xu, Zhe; Xiang, Yongyuan

    2016-01-01

    Minifilament eruptions (MFEs) and coronal jets are different types of solar small-scale explosive events. We report an MFE observed at the New Vacuum Solar Telescope (NVST). As seen in the NVST H α images, during the rising phase, the minifilament erupts outward orthogonally to its length, accompanied with a flare-like brightening at the bottom. Afterward, dark materials are found to possibly extend along the axis of the expanded filament body. The MFE is analogous to large filament eruptions. However, a simultaneous observation of the Solar Dynamics Observatory shows that a jet is initiated and flows out along nearby coronal loops during the rising phase of the MFE. Meanwhile, small hot loops, which connect the original eruptive site of the minifilament to the footpoints of the coronal loops, are formed successively. A differential emission measure analysis demonstrates that, on the top of the new small loops, a hot cusp structure exists. We conjecture that the magnetic fields of the MFE interact with magnetic fields of the coronal loops. This interaction is interpreted as magnetic reconnection that produces the jet and the small hot loops.

  6. Oblique Propagation and Dissipation of Alfvén Waves in Coronal ...

    Indian Academy of Sciences (India)

    velocity and energy flux density as the propagation angle of Alfvén waves increases inside the coronal holes. For any propagation angle, the energy flux density and damping length scale also show a decrement in the source region of the solar wind (<1.05 R⊙) where these may be one of the pri- mary energy sources ...

  7. Analysis of coronal H I Lyman alpha measurements from a rocket flight on 1979 April 13

    International Nuclear Information System (INIS)

    Withbroe, G.L.; Kohl, J.L.; Weiser, H.; Noci, G.; Munro, R.H.

    1982-01-01

    Measurements of the profiles of resonantly scattered hydrogen Lyman-α coronal radiation have been used to determine hydrogen kinetic temperatures from 1.5 to 4 R/sub sun/ from Sun center in a quiet region of the corona. Proton temperatures derived from the line widths decrease with height from 2.6 x 10 6 K at r = 1.5 R/sub sun/ to 1.2 x 10 6 K at r = 4 R/sub sun/. These measurements combined with temperatures for lower heights determined from earlier Skylab and eclipse data suggest that there is a maximum in the quiet coronal proton temperature at about 1.5 R/sub sun/. Comparison of measured Lyman-α intensities with those calculated using a representative model for the radial variation of the coronal electron density provides information on the magnitude of the electron temperature gradient and suggests that the solar wind flow was subsonic for r<4 R/sub sun/ in the observed region. Comparison of the measured kinetic temperatures to the predictions of a simple two fluid model suggests that there is a small amount of proton heating and/or a nonthermal contribution to the motions of coronal protons between 1.5 and 4 R/sub sun/

  8. ON THE CONNECTION BETWEEN PROPAGATING SOLAR CORONAL DISTURBANCES AND CHROMOSPHERIC FOOTPOINTS

    Energy Technology Data Exchange (ETDEWEB)

    Bryans, P.; McIntosh, S. W.; Moortel, I. De [High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307 (United States); Pontieu, B. De [Lockheed Martin Solar and Astrophysics Lab, Org. A021S, Bldg. 252, 3251 Hanover Street, Palo Alto, CA 94304 (United States)

    2016-09-20

    The Interface Region Imaging Spectrograph ( IRIS ) provides an unparalleled opportunity to explore the (thermal) interface between the chromosphere, transition region, and the coronal plasma observed by the Atmospheric Imaging Assembly (AIA) of the Solar Dynamics Observatory ( SDO ). The SDO /AIA observations of coronal loop footpoints show strong recurring upward propagating signals—“propagating coronal disturbances” (PCDs) with apparent speeds of the order of 100–120 km s{sup −1}. That signal has a clear signature in the slit-jaw images of IRIS in addition to identifiable spectral signatures and diagnostics in the Mg iih (2803 Å) line. In analyzing the Mg iih line, we are able to observe the presence of magnetoacoustic shock waves that are also present in the vicinity of the coronal loop footpoints. We see there is enough of a correspondence between the shock propagation in Mg iih, the evolution of the Si iv line profiles, and the PCD evolution to indicate that these waves are an important ingredient for PCDs. In addition, the strong flows in the jet-like features in the IRIS Si iv slit-jaw images are also associated with PCDs, such that waves and flows both appear to be contributing to the signals observed at the footpoints of PCDs.

  9. MULTIFRACTAL SOLAR EUV INTENSITY FLUCTUATIONS AND THEIR IMPLICATIONS FOR CORONAL HEATING MODELS

    Energy Technology Data Exchange (ETDEWEB)

    Cadavid, A. C.; Lawrence, J. K.; Christian, D. J. [Department of Physics and Astronomy, California State University Northridge, 18111 Nordhoff Street, Northridge, CA 91330 (United States); Rivera, Y. J. [Department of Climate and Space Sciences, University of Michigan, Ann Arbor, Michigan 48109-2143 (United States); Jennings, P. J. [5174 S. Slauson Avenue, Culver City, CA 90230 (United States); Rappazzo, A. F., E-mail: ana.cadavid@csun.edu [Department of Earth, Planetary and Space Sciences, University of California Los Angeles, Los Angeles, CA 90095 (United States)

    2016-11-10

    We investigate the scaling properties of the long-range temporal evolution and intermittency of Atmospheric Imaging Assembly/ Solar Dynamics Observatory intensity observations in four solar environments: an active region core, a weak emission region, and two core loops. We use two approaches: the probability distribution function (PDF) of time series increments and multifractal detrended fluctuation analysis (MF-DFA). Noise taints the results, so we focus on the 171 Å waveband, which has the highest signal-to-noise ratio. The lags between pairs of wavebands distinguish between coronal versus transition region (TR) emission. In all physical regions studied, scaling in the range of 15–45 minutes is multifractal, and the time series are anti-persistent on average. The degree of anti-correlation in the TR time series is greater than that for coronal emission. The multifractality stems from long-term correlations in the data rather than the wide distribution of intensities. Observations in the 335 Å waveband can be described in terms of a multifractal with added noise. The multiscaling of the extreme-ultraviolet data agrees qualitatively with the radiance from a phenomenological model of impulsive bursts plus noise, and also from ohmic dissipation in a reduced magnetohydrodynamic model for coronal loop heating. The parameter space must be further explored to seek quantitative agreement. Thus, the observational “signatures” obtained by the combined tests of the PDF of increments and the MF-DFA offer strong constraints that can systematically discriminate among models for coronal heating.

  10. Spectroscopic observations of Nova Cygni 1975: The coronal line region revisited

    International Nuclear Information System (INIS)

    Ferland, G.J.; Lambert, D.L.; Woodman, J.H.

    1986-01-01

    A synopsis of the McDonald Observatory spectrophotometric observations of Nova Cyg 1975 (V1500 Cyg) is presented. We present these data in a form in which they can be readily accessed in the future, and also study the continous spectrum during the early nebular phase. We show that (1) the remnant probably maintained a luminosity at or above the Eddington limit for at least a year after outburst, (2) free-free emission from the coronal line region made a significant contribution to the optical continuum, and (3) the coronal line region was probably a significant source of ionizing radiation. The energetics of this nova appear to be dominated by the lift-off energy from the white dwarf and radiation from the coronal line region. Thus the light curve of Nova Cyg may tell more about the cooling of the coronal line region than about the decline of the central object. In appendices we discuss the argon abundance of Nova Cyg (less than 8 times solar) and describe how to obtain copies of the McDonald nova data

  11. MINI-FILAMENT ERUPTION AS THE INITIATION OF A JET ALONG CORONAL LOOPS

    Energy Technology Data Exchange (ETDEWEB)

    Hong, Junchao; Jiang, Yunchun; Yang, Jiayan; Yang, Bo; Xu, Zhe; Xiang, Yongyuan, E-mail: hjcsolar@ynao.ac.cn [Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011 (China)

    2016-10-20

    Minifilament eruptions (MFEs) and coronal jets are different types of solar small-scale explosive events. We report an MFE observed at the New Vacuum Solar Telescope (NVST). As seen in the NVST H α images, during the rising phase, the minifilament erupts outward orthogonally to its length, accompanied with a flare-like brightening at the bottom. Afterward, dark materials are found to possibly extend along the axis of the expanded filament body. The MFE is analogous to large filament eruptions. However, a simultaneous observation of the Solar Dynamics Observatory shows that a jet is initiated and flows out along nearby coronal loops during the rising phase of the MFE. Meanwhile, small hot loops, which connect the original eruptive site of the minifilament to the footpoints of the coronal loops, are formed successively. A differential emission measure analysis demonstrates that, on the top of the new small loops, a hot cusp structure exists. We conjecture that the magnetic fields of the MFE interact with magnetic fields of the coronal loops. This interaction is interpreted as magnetic reconnection that produces the jet and the small hot loops.

  12. The environment of the sun during the explosion of Coronal Mass ...

    African Journals Online (AJOL)

    Coronal Mass Ejections (CMEs) have been studied has become the most important phenomena of solar activity because it is the most energetic phenomena on the Sun. Concerning the importance of the impact of solar radio burst, we study the selected event of CMEs to observe the environment of the atmosphere of the ...

  13. Exploring Coronal Structures with SOHO Μ. Karovska1*, Β. Wood1 ...

    Indian Academy of Sciences (India)

    tribpo

    Astr. (2000) 21, 403–406. Exploring Coronal ... et al. 1995). The wavelengths and the dominant emission lines in these bandpasses ... (2) the profile of the poloidal flux injection (Chen et al. 1997 ... Delaboudiniere, J. P., et al, 1995, Sol. Phys.

  14. DESCRIPCIÓN DE LOS ESTUDIOS POSAUTORIZACIÓN OBSERVACIONALES PROSPECTIVOS CON MEDICAMENTOS EN LA COMUNITAT VALENCIANA ENTRE 2010 Y 2015. ANÁLISIS DE LOS FACTORES RELACIONADOS CON SU AUTORIZACIÓN

    Directory of Open Access Journals (Sweden)

    María Antonia Grau Rubio

    2017-01-01

    Full Text Available Fundamentos: Los estudios posautorización observacionales son una fuente de información clave sobre efectividad y seguridad de los medica - mentos. Los objetivos del estudio fueron describir las características de los estudios observacionales de seguimiento prospectivo (EPA-SP que solicita - ron autorización en la Comunitat Valenciana (CV y explorar qué factores se asociaron con su autorización. Métodos: Se realizó estudio observacional analítico retrospectivo, en el que se incluyeron todos los EPA-SP que solicitaron autorización en la CV desde 2010 hasta 2015. A partir de las bases de datos de la Dirección Ge - neral de Farmacia y Productos Sanitarios y GESTO se obtuvieron variables referentes al estudio (objetivos, medicamento estudiado, enfermedad diana, etc y referentes al procedimiento de autorización (autorización, motivo de no autorización y estado actual del estudio. El análisis se organizó en una fase descriptiva y otra analítica mediante regresión logística con variable dependiente la autorización. Resultados: Fueron incluidos un total de 249 estudios, de los que 192 (77,1% estaban diseñados para estimar efectividad o calidad de vida. Los medicamentos más frecuentemente estudiados fueron los agentes anti - neoplásicos e inmunomoduladores (42%. Sólo consiguieron la autorización el 57%, siendo las causas más frecuente de denegación la inducción a la prescripción (40,1% y la práctica no habitual (39,3%. La autorización se asoció con el diagnóstico (aparato circulatorio OR 10,7, IC95% 2,3 a 49,1, grupo ATC L (OR 4,2, IC95% 1,9 a 49,1 y el haber sido promovidos por la industria (OR 0,5, IC95% 0,3 a 0,9. Conclusión: Dada la importancia de contar con información sobre efec - tividad y seguridad en la práctica habitual, es prioritario que los EPA-SP sean orientados a estos fines y que se potencie la investigación independiente.

  15. Pediatric HIV-related oral manifestations: a five-year retrospective study Manifestações bucais associadas à infecção pelo HIV em crianças: estudo retrospectivo de cinco anos

    Directory of Open Access Journals (Sweden)

    Lívia Ferreira Soares

    2004-03-01

    Full Text Available The purpose of this study was to carry out a five-year retrospective descriptive follow-up of the oral manifestation frequency, systemic condition and type of medication used in HIV-infected children and adolescents after the introduction of combined antiretroviral therapy. Fifty-eight patients were examined in 2001/2002, and their previous medical and dental records (1997 to 2000 were researched from files. There was an occurrence of 7 new cases of AIDS in a sample of 19 children, while 46.5% of the entire sample (n = 58 progressed as to classification of HIV infection. No difference was noted among the frequencies of oral manifestations, categories of the immunosuppression and viral load categories. The oral manifestations in the group of children and adolescents followed up in this study remained stable, even after treatment with combined antiretroviral therapy. However, a downward trend in the frequency of oral candidiasis and parotid enlargement was noted.O objetivo deste estudo foi realizar um acompanhamento descritivo retrospectivo da freqüência de manifestações bucais, da condição sistêmica e do tipo de medicação utilizada em um grupo de crianças e adolescentes infectados pelo HIV após a introdução da terapia anti-retroviral combinada. Cinqüenta e oito pacientes foram examinados em 2001/2002, enquanto seus exames médicos e odontológicos retrospectivos (1997 a 2000 foram pesquisados em prontuário. Foram observados 7 novos casos de AIDS em uma amostra de 19 pacientes, enquanto 46,5% da amostra total (n = 58 progrediram quanto à classificação da infecção pelo HIV. Não foram observadas diferenças entre as freqüências de manifestações bucais, das categorias de imunossupressão e da carga viral. O quadro de manifestações bucais no grupo de crianças e adolescentes acompanhados neste estudo manteve-se estável, mesmo após a introdução da terapia anti-retroviral combinada. Contudo, foi observada uma tendência de

  16. Tuberculosis en trabajadores de salud: Estudio epidemiológico y clínico en el Hospital Nacional Hipólito Unanue

    Directory of Open Access Journals (Sweden)

    Mayron Nakandakari

    2014-07-01

    Full Text Available Objetivo: Describir las características epidemiológicas y clínicas de los trabajadores de salud del Hospital Nacional Hipólito Unanue (HNHU con diagnóstico de Tuberculosis (TBC entre el 2006 y 2013. Material y métodos: Estudio observacional, descriptivo, longitudinal, retrospectivo, realizado en el HNHU de categoría III-1. La población estudiada estuvo constituida por los trabajadores de salud con diagnóstico de Tuberculosis entre el 2006 y el 2013. La muestra fue todo el universo. La técnica fue de documentación. Se utilizó estadística descriptiva y los programas Microsoft Excel 2010 y SPSS v 19. Resultados: Se identificaron 56 trabajadores de Salud con diagnóstico de TBC, 4 fueron BK (+++ y uno falleció. La frecuencia de los casos tuvo una tendencia a disminuir desde el 2008, con su valor más bajo en el 2012. Conclusiones: La mayoría fueron diagnosticados en el 2007 y 2013, médicos residentes, BK negativo, con TBC pulmonar sensible y del Servicio de Hospitalización de Especialidades

  17. Infrared Dual-Line Hanle Diagnostic of the Coronal Vector Magnetic Field

    Energy Technology Data Exchange (ETDEWEB)

    Dima, Gabriel I.; Kuhn, Jeffrey R. [Institute for Astronomy, University of Hawaii, Pukalani, HI (United States); Berdyugina, Svetlana V., E-mail: gdima@hawaii.edu [Institute for Astronomy, University of Hawaii, Pukalani, HI (United States); Kiepenheuer Institut fuer Sonnenphysik, Freiburg (Germany); Predictive Science Inc., San Diego, CA (United States)

    2016-04-20

    Measuring the coronal vector magnetic field is still a major challenge in solar physics. This is due to the intrinsic weakness of the field (e.g., ~4G at a height of 0.1R⊙ above an active region) and the large thermal broadening of coronal emission lines. We propose using concurrent linear polarization measurements of near-infrared forbidden and permitted lines together with Hanle effect models to calculate the coronal vector magnetic field. In the unsaturated Hanle regime both the direction and strength of the magnetic field affect the linear polarization, while in the saturated regime the polarization is insensitive to the strength of the field. The relatively long radiative lifetimes of coronal forbidden atomic transitions implies that the emission lines are formed in the saturated Hanle regime and the linear polarization is insensitive to the strength of the field. By combining measurements of both forbidden and permitted lines, the direction and strength of the field can be obtained. For example, the SiX 1.4301 μm line shows strong linear polarization and has been observed in emission over a large field-of-view (out to elongations of 0.5 R⊙). Here we describe an algorithm that combines linear polarization measurements of the SiX 1.4301 μm forbidden line with linear polarization observations of the HeI 1.0830 μm permitted coronal line to obtain the vector magnetic field. To illustrate the concept we assume that the emitting gas for both atomic transitions is located in the plane of the sky. The further development of this method and associated tools will be a critical step toward interpreting the high spectral, spatial and temporal infrared spectro-polarimetric measurements that will be possible when the Daniel K. Inouye Solar Telescope (DKIST) is completed in 2019.

  18. OBSERVATIONAL SIGNATURES OF CORONAL LOOP HEATING AND COOLING DRIVEN BY FOOTPOINT SHUFFLING

    Energy Technology Data Exchange (ETDEWEB)

    Dahlburg, R. B.; Taylor, B. D. [LCP and FD, Naval Research Laboratory, Washington, DC 20375 (United States); Einaudi, G. [Berkeley Research Associates, Inc., Beltsville, MD 20705 (United States); Ugarte-Urra, I. [College of Science, George Mason University, Fairfax, VA 22030 (United States); Warren, H. P. [Space Science Division, Naval Research Laboratory, Washington, DC 20375 (United States); Rappazzo, A. F. [Advanced Heliophysics, Pasadena, CA 91106 (United States); Velli, M., E-mail: rdahlbur@lcp.nrl.navy.mil [EPSS, UCLA, Los Angeles, CA 90095 (United States)

    2016-01-20

    The evolution of a coronal loop is studied by means of numerical simulations of the fully compressible three-dimensional magnetohydrodynamic equations using the HYPERION code. The footpoints of the loop magnetic field are advected by random motions. As a consequence, the magnetic field in the loop is energized and develops turbulent nonlinear dynamics characterized by the continuous formation and dissipation of field-aligned current sheets: energy is deposited at small scales where heating occurs. Dissipation is nonuniformly distributed so that only a fraction of the coronal mass and volume gets heated at any time. Temperature and density are highly structured at scales that, in the solar corona, remain observationally unresolved: the plasma of our simulated loop is multithermal, where highly dynamical hotter and cooler plasma strands are scattered throughout the loop at sub-observational scales. Numerical simulations of coronal loops of 50,000 km length and axial magnetic field intensities ranging from 0.01 to 0.04 T are presented. To connect these simulations to observations, we use the computed number densities and temperatures to synthesize the intensities expected in emission lines typically observed with the Extreme Ultraviolet Imaging Spectrometer on Hinode. These intensities are used to compute differential emission measure distributions using the Monte Carlo Markov Chain code, which are very similar to those derived from observations of solar active regions. We conclude that coronal heating is found to be strongly intermittent in space and time, with only small portions of the coronal loop being heated: in fact, at any given time, most of the corona is cooling down.

  19. The Three-part Structure of a Filament-unrelated Solar Coronal Mass Ejection

    Energy Technology Data Exchange (ETDEWEB)

    Song, H. Q.; Chen, Y.; Wang, B.; Li, B. [Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, and Institute of Space Sciences, Shandong University, Weihai, Shandong 264209 (China); Cheng, X. [School of Astronomy and Space Science, Nanjing University, Nanjing, Jiangsu 210093 (China); Zhang, J. [Department of Physics and Astronomy, George Mason University, Fairfax, VA 22030 (United States); Li, L. P. [Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); Hu, Q.; Li, G., E-mail: hqsong@sdu.edu.cn [Department of Space Science and CSPAR, University of Alabama in Huntsville, AL 35899 (United States)

    2017-10-10

    Coronal mass ejections (CMEs) often exhibit the typical three-part structure in the corona when observed with white-light coronagraphs, i.e., the bright leading front, dark cavity, and bright core, corresponding to a high-low-high density sequence. As CMEs result from eruptions of magnetic flux ropes (MFRs), which can possess either lower (e.g., coronal-cavity MFRs) or higher (e.g., hot-channel MFRs) density compared to their surroundings in the corona, the traditional opinion regards the three-part structure as the manifestations of coronal plasma pileup (high density), coronal-cavity MFR (low density), and filament (high density) contained in the trailing part of MFR, respectively. In this paper, we demonstrate that filament-unrelated CMEs can also exhibit the classical three-part structure. The observations were made from different perspectives through an event that occurred on 2011 October 4. The CME cavity corresponds to the low-density zone between the leading front and the high-density core, and it is obvious in the low corona and gradually becomes fuzzy when propagating outward. The bright core corresponds to a high-density structure that is suggested to be an erupting MFR. The MFR is recorded from both edge-on and face-on perspectives, exhibiting different morphologies that are due to projection effects. We stress that the zone (MFR) with lower (higher) density in comparison to the surroundings can appear as the dark cavity (bright core) when observed through white-light coronagraphs, which is not necessarily the coronal-cavity MFR (erupted filament).

  20. The Medical Examiner/Coroner's Guide for Contaminated Deceased Body Management.

    Science.gov (United States)

    Hanzlick, Randy; Nolte, Kurt; deJong, Joyce

    2009-12-01

    In the past few years, a number of publications and other resources have appeared concerning the management of mass fatality incidents. Some are geared toward the general management of incidents while others cover more specific topics such as decontamination procedures. Still others cover selected agents, including chemical, biologic, or radiologic ones. Few publications have been written specifically for medical examiners and coroners. The Medical Examiner and Coroner's Guide for Contaminated Deceased Body Management is written specifically for the medical examiner or coroner who will be in charge of investigations of fatalities that result from terrorism or other events that result in contaminated remains. In some such cases, agents may be used that will require mitigation of environmental hazards and decontamination of human bodies. To that end, this Guide provides information and suggestions that may be useful in understanding the principles involved in decontamination procedures, recognizing that it may not be the medical examiner or coroner staff who actually conducts decontamination procedures. The suggestions in this guide may differ slightly from those in other publications. However, those who have contributed to this guide believe that the recommendations are practical, workable, have a scientific basis, and do not differ much in substance when compared with other relevant publications. The contents of this Guide may be reproduced for practical use but the Guide may not be sold and it may not be cited for advertisement purposes. Reference to specific commercial products is for informational purposes only and does not constitute endorsement of the product or company which produces the product. The recommendations contained in this Guide are not mandated nor are they required by federal, state, or local law. Rather, the recommendations are intended to assist medical examiners and coroners for the purposes of planning and providing a set of reasonable

  1. Coronal mass ejections and disturbances in solar wind plasma parameters in relation with geomagnetic storms

    International Nuclear Information System (INIS)

    Verma, P L; Singh, Puspraj; Singh, Preetam

    2014-01-01

    Coronal Mass Ejections (CMEs) are the drastic solar events in which huge amount of solar plasma materials are ejected into the heliosphere from the sun and are mainly responsible to generate large disturbances in solar wind plasma parameters and geomagnetic storms in geomagnetic field. We have studied geomagnetic storms, (Dst ≤-75 nT) observed during the period of 1997-2007 with Coronal Mass Ejections and disturbances in solar wind plasma parameters (solar wind temperature, velocity, density and interplanetary magnetic field) .We have inferred that most of the geomagnetic storms are associated with halo and partial halo Coronal Mass Ejections (CMEs).The association rate of halo and partial halo coronal mass ejections are found 72.37 % and 27.63 % respectively. Further we have concluded that geomagnetic storms are closely associated with the disturbances in solar wind plasma parameters. We have determined positive co-relation between magnitudes of geomagnetic storms and magnitude of jump in solar wind plasma temperature, jump in solar wind plasma density, jump in solar wind plasma velocity and jump in average interplanetary magnetic field with co-relation co-efficient 0 .35 between magnitude of geomagnetic storms and magnitude of jump in solar wind plasma temperature, 0.19 between magnitude of geomagnetic storms and magnitude of jump in solar wind density, 0.34 between magnitude of geomagnetic storms and magnitude of jump in solar wind plasma velocity, 0.66 between magnitude of geomagnetic storms and magnitude of jump in average interplanetary magnetic field respectively. We have concluded that geomagnetic storms are mainly caused by Coronal Mass Ejections and disturbances in solar wind plasma parameters that they generate.

  2. The Three-part Structure of a Filament-unrelated Solar Coronal Mass Ejection

    International Nuclear Information System (INIS)

    Song, H. Q.; Chen, Y.; Wang, B.; Li, B.; Cheng, X.; Zhang, J.; Li, L. P.; Hu, Q.; Li, G.

    2017-01-01

    Coronal mass ejections (CMEs) often exhibit the typical three-part structure in the corona when observed with white-light coronagraphs, i.e., the bright leading front, dark cavity, and bright core, corresponding to a high-low-high density sequence. As CMEs result from eruptions of magnetic flux ropes (MFRs), which can possess either lower (e.g., coronal-cavity MFRs) or higher (e.g., hot-channel MFRs) density compared to their surroundings in the corona, the traditional opinion regards the three-part structure as the manifestations of coronal plasma pileup (high density), coronal-cavity MFR (low density), and filament (high density) contained in the trailing part of MFR, respectively. In this paper, we demonstrate that filament-unrelated CMEs can also exhibit the classical three-part structure. The observations were made from different perspectives through an event that occurred on 2011 October 4. The CME cavity corresponds to the low-density zone between the leading front and the high-density core, and it is obvious in the low corona and gradually becomes fuzzy when propagating outward. The bright core corresponds to a high-density structure that is suggested to be an erupting MFR. The MFR is recorded from both edge-on and face-on perspectives, exhibiting different morphologies that are due to projection effects. We stress that the zone (MFR) with lower (higher) density in comparison to the surroundings can appear as the dark cavity (bright core) when observed through white-light coronagraphs, which is not necessarily the coronal-cavity MFR (erupted filament).

  3. The Three-part Structure of a Filament-unrelated Solar Coronal Mass Ejection

    Science.gov (United States)

    Song, H. Q.; Cheng, X.; Chen, Y.; Zhang, J.; Wang, B.; Li, L. P.; Li, B.; Hu, Q.; Li, G.

    2017-10-01

    Coronal mass ejections (CMEs) often exhibit the typical three-part structure in the corona when observed with white-light coronagraphs, I.e., the bright leading front, dark cavity, and bright core, corresponding to a high-low-high density sequence. As CMEs result from eruptions of magnetic flux ropes (MFRs), which can possess either lower (e.g., coronal-cavity MFRs) or higher (e.g., hot-channel MFRs) density compared to their surroundings in the corona, the traditional opinion regards the three-part structure as the manifestations of coronal plasma pileup (high density), coronal-cavity MFR (low density), and filament (high density) contained in the trailing part of MFR, respectively. In this paper, we demonstrate that filament-unrelated CMEs can also exhibit the classical three-part structure. The observations were made from different perspectives through an event that occurred on 2011 October 4. The CME cavity corresponds to the low-density zone between the leading front and the high-density core, and it is obvious in the low corona and gradually becomes fuzzy when propagating outward. The bright core corresponds to a high-density structure that is suggested to be an erupting MFR. The MFR is recorded from both edge-on and face-on perspectives, exhibiting different morphologies that are due to projection effects. We stress that the zone (MFR) with lower (higher) density in comparison to the surroundings can appear as the dark cavity (bright core) when observed through white-light coronagraphs, which is not necessarily the coronal-cavity MFR (erupted filament).

  4. ESTUDIOS TRANSCULTURALES DEL BURNOUT: LOS ESTUDIOS TRANSCULTURALES BRASIL-ESPAÑA

    Directory of Open Access Journals (Sweden)

    Macarena Gálvez Herrer

    2003-07-01

    Full Text Available Los estudios transculturales no son un ejercicio secundario y complementario en el estudio de la psicología; un modelo antropológico de la conducta humana obliga a plantear que las variables culturales no son secundarias sino primarias. Por estas razones el estudio del “burnout†o desgaste profesional puede profundizarse mediante la utilización de los métodos transculturales. No es suficiente con la simple comparación de resultados, sino que es necesario buscar instrumentos propios de cada cultura y establecer la comparación no sólo del síndrome de desgaste profesional sino de todos los diferentes elementos del proceso. El trabajo presentado establece las bases teóricas de este planteamiento, y expone, mediante un ejemplo, algunas de las vías posibles para una psicología transcultural del burnout.

  5. Estudios transculturales del burnout: Los estudios transculturales Brasil-España

    Directory of Open Access Journals (Sweden)

    Bernardo Moreno Jiménez

    2003-01-01

    Full Text Available Los estudios transculturales no son un ejercicio secundario y complementario en el estudio de la psicología; un modelo antropológico de la conducta humana obliga a plantear que las variables culturales no son secundarias sino primarias. Por estas razones el estudio del “burnout” o desgaste profesional puede profundizarse mediante la utilización de los métodos transculturales. No es suficiente con la simple comparación de resultados, sino que es necesario buscar instrumentos propios de cada cultura y establecer la comparación no sólo del síndrome de desgaste profesional sino de todos los diferentes elementos del proceso. El trabajo presentado establece las bases teóricas de este planteamiento, y expone, mediante un ejemplo, algunas de las vías posibles para una psicología transcultural del burnout

  6. Fracture morphology of AO/OTA 31-A trochanteric fractures: A 3D CT study with an emphasis on coronal fragments.

    Science.gov (United States)

    Cho, Jae-Woo; Kent, William T; Yoon, Yong-Cheol; Kim, Youngwoo; Kim, Hyungon; Jha, Ashutosh; Durai, Senthil Kumar; Oh, Jong-Keon

    2017-02-01

    This study was designed to assess the incidence and morphology of coronal plane fragments in AO/OTA 31-A trochanteric fractures. 156 cases of AO/OTA 31-A trochanteric fractures were retrospectively evaluated. Lateral radiographs were analyzed for the presence of coronal plane fragments followed by analysis of 3D CT reconstructions in these fractures. The incidence of coronal fragments identified on the lateral radiograph and 3D CT reconstructions were both calculated. Coronal fragment morphology was described based upon the origin and exit points of fracture lines and the number of fragments. On plain radiographs, a coronal plane fracture was identified in 59 cases, an incidence of 37.8% (59/156). In comparison, 3D CT reconstructions identified coronal plane fractures in 138 cases for an incidence of 88.4% (138/156). 3D CT reconstructions identified coronal fracture fragments in 81.9% (50/61) of AO/OTA 31-A1 cases, 94.5% (69/73) of 31-A2 cases, and 86.3% (19/22) of 31-A3 cases. Incidence of coronal fractures identified on plain radiographs of 3 AO/OTA 31-A1,A2,A3 groups was lower when compared to the incidence of coronal fractures identified on 3D CT. Of the 138 cases that had coronal plane fracture, 82 cases (59.4%) had a single coronal fragment (GT fragment 35 cases, GLT fragment 19 cases, GLPC fragment 28 cases). The remaining 56 cases (40.5%) had two coronal fragments. There is a high incidence of coronal fragments in intertrochanteric femur fractures when analyzed with 3D CT reconstructions. Our study suggests that these coronal fragments are difficult to identify on plain radiographs. Knowledge of the incidence and morphology of coronal fragments helps to avoid potential intraoperative pitfalls. Copyright © 2016 Elsevier Ltd. All rights reserved.

  7. Coronal 2D MR cholangiography overestimates the length of the right hepatic duct in liver transplantation donors

    International Nuclear Information System (INIS)

    Kim, Bohyun; Kim, Kyoung Won; Kim, So Yeon; Park, So Hyun; Lee, Jeongjin; Song, Gi Won; Jung, Dong-Hwan; Ha, Tae-Yong; Lee, Sung Gyu

    2017-01-01

    To compare the length of the right hepatic duct (RHD) measured on rotatory coronal 2D MR cholangiography (MRC), rotatory axial 2D MRC, and reconstructed 3D MRC. Sixty-seven donors underwent coronal and axial 2D projection MRC and 3D MRC. RHD length was measured and categorized as ultrashort (≤1 mm), short (>1-14 mm), and long (>14 mm). The measured length, frequency of overestimation, and the degree of underestimation between two 2D MRC sets were compared to 3D MRC. The length of the RHD from 3D MRC, coronal 2D MRC, and axial 2D MRC showed significant difference (p < 0.05). RHD was frequently overestimated on the coronal than on axial 2D MRC (61.2 % vs. 9 %; p <.0001). On coronal 2D MRC, four (6 %) with short RHD and one (1.5 %) with ultrashort RHD were over-categorized as long RHD. On axial 2D MRC, overestimation was mostly <1 mm (83.3 %), none exceeding 3 mm or over-categorized. The degree of underestimation between the two projection planes was comparable. Coronal 2D MRC overestimates the RHD in liver donors. We suggest adding axial 2D MRC to conventional coronal 2D MRC in the preoperative workup protocol for living liver donors to avoid unexpected confrontation with multiple ductal openings when harvesting the graft. (orig.)

  8. Impulsively Generated Wave Trains in Coronal Structures. II. Effects of Transverse Structuring on Sausage Waves in Pressurelesss Slabs

    Science.gov (United States)

    Li, Bo; Guo, Ming-Zhe; Yu, Hui; Chen, Shao-Xia

    2018-03-01

    Impulsively generated sausage wave trains in coronal structures are important for interpreting a substantial number of observations of quasi-periodic signals with quasi-periods of order seconds. We have previously shown that the Morlet spectra of these wave trains in coronal tubes depend crucially on the dispersive properties of trapped sausage waves, the existence of cutoff axial wavenumbers, and the monotonicity of the dependence of the axial group speed on the axial wavenumber in particular. This study examines the difference a slab geometry may introduce, for which purpose we conduct a comprehensive eigenmode analysis, both analytically and numerically, on trapped sausage modes in coronal slabs with a considerable number of density profiles. For the profile descriptions examined, coronal slabs can trap sausage waves with longer axial wavelengths, and the group speed approaches the internal Alfvén speed more rapidly at large wavenumbers in the cylindrical case. However, common to both geometries, cutoff wavenumbers exist only when the density profile falls sufficiently rapidly at distances far from coronal structures. Likewise, the monotonicity of the group speed curves depends critically on the profile steepness right at the structure axis. Furthermore, the Morlet spectra of the wave trains are shaped by the group speed curves for coronal slabs and tubes alike. Consequently, we conclude that these spectra have the potential for inferring the subresolution density structuring inside coronal structures, although their detection requires an instrumental cadence of better than ∼1 s.

  9. Coronal 2D MR cholangiography overestimates the length of the right hepatic duct in liver transplantation donors

    Energy Technology Data Exchange (ETDEWEB)

    Kim, Bohyun [University of Ulsan College of Medicine, Department of Radiology, Asan Medical Center, 88, Olympic-ro 43-gil, Songpa-gu, Seoul (Korea, Republic of); Ajou University School of Medicine, Department of Radiology, Ajou University Medical Center, Suwon (Korea, Republic of); Kim, Kyoung Won; Kim, So Yeon; Park, So Hyun [University of Ulsan College of Medicine, Department of Radiology, Asan Medical Center, 88, Olympic-ro 43-gil, Songpa-gu, Seoul (Korea, Republic of); Lee, Jeongjin [Soongsil University, School of Computer Science and Engineering, Seoul (Korea, Republic of); Song, Gi Won; Jung, Dong-Hwan; Ha, Tae-Yong; Lee, Sung Gyu [University of Ulsan College of Medicine, Department of Surgery, Division of Hepatobiliary and Liver Transplantation Surgery, Asan Medical Center, Seoul (Korea, Republic of)

    2017-05-15

    To compare the length of the right hepatic duct (RHD) measured on rotatory coronal 2D MR cholangiography (MRC), rotatory axial 2D MRC, and reconstructed 3D MRC. Sixty-seven donors underwent coronal and axial 2D projection MRC and 3D MRC. RHD length was measured and categorized as ultrashort (≤1 mm), short (>1-14 mm), and long (>14 mm). The measured length, frequency of overestimation, and the degree of underestimation between two 2D MRC sets were compared to 3D MRC. The length of the RHD from 3D MRC, coronal 2D MRC, and axial 2D MRC showed significant difference (p < 0.05). RHD was frequently overestimated on the coronal than on axial 2D MRC (61.2 % vs. 9 %; p <.0001). On coronal 2D MRC, four (6 %) with short RHD and one (1.5 %) with ultrashort RHD were over-categorized as long RHD. On axial 2D MRC, overestimation was mostly <1 mm (83.3 %), none exceeding 3 mm or over-categorized. The degree of underestimation between the two projection planes was comparable. Coronal 2D MRC overestimates the RHD in liver donors. We suggest adding axial 2D MRC to conventional coronal 2D MRC in the preoperative workup protocol for living liver donors to avoid unexpected confrontation with multiple ductal openings when harvesting the graft. (orig.)

  10. ESTUDIO DE FRACCIONES EN CONTEXTOS SONOROS

    Directory of Open Access Journals (Sweden)

    Alexander Conde

    2016-01-01

    Full Text Available En este ensayo resaltamos los vínculos cognitivos entre las matemáticas y la música, que pueden favorecer procesos de enseñanza y aprendizaje de las fracciones en la matemática escolar. Las actividades exhibidas provienen de una investigación que promueve experiencias sensoriales en el campo rítmico para favorecer la construcción de nociones matemáticas. Dichas actividades posibilitan un engranaje armónico entre las matemáticas y la música convergentes en el tiempo y el sonido como los objetos de estudio común entre éstas disciplinas. El análisis de la investigación que aquí reportamos es producto de la aplicación de las actividades en diferentes programas de formación de profesorado de México y Francia, alrededor de la enseñanza y aprendizaje de las matemáticas en contextos interdisciplinarios. Este análisis se desarrolló desde tres categorías referentes a las nociones de unidad relativa, relación parte-parte y equipartición, las cuales son nociones fundamentales para el estudio de las fracciones en la matemática escolar. Encontramos que la enseñanza con enfoque integrador requiere no solo conocimientos especializados, sino un cambio de creencias en torno a las opiniones del profesorado sobre la organización del currículo, su enseñanza y la manera en que aprende la población estudiantil. Un aporte de esta experiencia es ofrecer a docentes elementos teóricos y didácticos para el estudio de las fracciones en contextos interdisciplinarios.

  11. Pênfigo foliáceo canino: estudo retrospectivo de 43 casos clínicos e terapia (2000-2005 Canine Pemphigus foliaceus: a retrospective study of 43 clinical cases and therapy (2000-2005

    Directory of Open Access Journals (Sweden)

    Ana C. Balda

    2008-08-01

    Full Text Available No período de agosto de 2000 a julho de 2005 foram atendidos 43 casos de Pênfigo Foliáceo (PF canino no Serviço de Dermatologia do Hospital Veterinária, Universidade de São Paulo. Com este estudo retrospectivo visou-se atualizar dados referentes à caracterização sexual, definição racial e raça, idade, tipo e topografia lesional, quadro sintomático e resposta aos tratamentos isolados com prednisona e com a associação desta à azatioprina, além de demonstrar o aumento na ocorrência do PF relativamente à série histórica pretérita (1986-2000 do mesmo Serviço.From August 2000 to July 2005 were attended 43 cases of canine Pemphigus foliaceous (PF by the Dermatology Service of the Veterinary Teaching Hospital, University of São Paulo. The aim of the present study was to update the records referred to sex, breed, age, type and location of the lesions, clinical signs, and response to treatments with prednisone or combination with prednisone and azathioprine, and also to demonstrate the increase of occurrence of PF compared with the former series (1986-2000 observed in the same Service.

  12. Estudio de un caso de control interno

    OpenAIRE

    Alfonso Pirela

    2005-01-01

    El estudio se efectuó con el objetivo de analizar el control interno en el Almacén de la Facultad de ciencias Económicas y Sociales de la Universidad del Zulia. La metodología fue descriptiva. Se utilizó como población a todo el personal del almacén. Los resultados arrojaron que el control del almacén no cuenta con un sistema de control interno integrado que le permita llevar con efectividad las actividades de recepción, almacenamiento y despacho de la mercancía.

  13. Estudio de un caso de control interno

    Directory of Open Access Journals (Sweden)

    Alfonso Pirela

    2005-09-01

    Full Text Available El estudio se efectuó con el objetivo de analizar el control interno en el Almacén de la Facultad de ciencias Económicas y Sociales de la Universidad del Zulia. La metodología fue descriptiva. Se utilizó como población a todo el personal del almacén. Los resultados arrojaron que el control del almacén no cuenta con un sistema de control interno integrado que le permita llevar con efectividad las actividades de recepción, almacenamiento y despacho de la mercancía.

  14. Estudio sobre redes sociales y estudiantes

    OpenAIRE

    Toledo Morales, Purificación; Sánchez García, José Manuel

    2012-01-01

    En este estudio pretendemos analizar cómo una muestra de 150 estudiantes utiliza las redes sociales, y explorar el impacto de estas en el rendimiento académico de los mismos. Los datos recogidos de la aplicación y análisis de una escala de opinión revelaron que mas de la mitad de los estudiantes encuestados utilizan internet con una finalidad puramente recreativa, y las redes sociales para estar en contacto con los amigos. La mayoría de los encuestados rechazan las solicitudes de amistad de d...

  15. Amplificadores con transistores. Estudio y dimensionado

    OpenAIRE

    Lubiano García, Adrián

    2017-01-01

    Este trabajo es un estudio de las distintas configuraciones de los amplificadores con transistores vistos en la asignatura de Electrónica Analógica del tercer curso del Grado en Ingeniería en Electrónica Industrial y Automática de la Escuela de Ingenierías Industriales de la Universidad de Valladolid. En este trabajo se mostrarán los pasos seguidos en la creación de una aplicación con Visual Basic para la realización de los ejercicios de las distintas configuraciones, así...

  16. Estudio del álbum sin palabras

    OpenAIRE

    Bosch Andreu, Emma

    2015-01-01

    [spa] Estudio del Álbum Sin Palabras tiene como objetivo principal definir, analizar y categorizar los álbumes sin palabras destinados principalmente al público infantil y juvenil dando a conocer sus características, peculiariades y diversidad tipológica, para facilitar las tareas de análisis y de mediación de investigadores, educadores, bibliotecarios y cualquier persona interesada en los libros con imágenes. En el capítulo titulado «Un nuevo mapa para los Libros Sin Palabras» situamos e...

  17. Anorexia nervosa: un estudio de casos

    OpenAIRE

    Zusman, Lillyana

    2013-01-01

    La Anorexia Nervosa es un trastorno de alimentación que se define (etimológicamente) como una "pérdida nerviosa del apetito". Se caracteriza por la actitud consciente, voluntaria y rotunda de los sujetos  de tener un exceso de peso que intentan modificar por vía de la inanición. A partir del estudio de casos, se propone la distinción entre una Anorexia Nervosa Estructural -aquella en la que predomina el conflicto intrapsíquico primario y arcaico, y que manifiesta una conducta aislada y retraí...

  18. Improving tibial component coronal alignment during total knee arthroplasty with use of a tibial planing device.

    Science.gov (United States)

    Patil, Shantanu; D'Lima, Darryl D; Fait, James M; Colwell, Clifford W

    2007-02-01

    The outcomes of knee arthroplasty have been shown to be affected by component alignment. Intramedullary and extramedullary alignment instrumentation are fairly effective for achieving the desired mean tibial component coronal alignment. However, there are outliers representing >3 degrees of varus or valgus alignment with respect to the anatomic tibial shaft axis. We measured the efficacy of a custom tibial planing device for reducing the outliers in tibial alignment. We designed a tibial planing tool in an effort to improve tibial alignment. In one cohort (100 knees), we used traditional intramedullary alignment instrumentation to make the tibial bone cut. In a second cohort (120 knees), we used intramedullary alignment instrumentation to make the cut and also used a custom tool to check the cut and to correct an inexact cut. Tibial tray alignment relative to the long axis of the tibial shaft was measured in the coronal and sagittal planes on postoperative radiographs. The target coronal alignment was 90 degrees with respect to the tibial shaft axis (with alignment). A total of 100 anteroposterior radiographs and sixty-five lateral radiographs were analyzed for the group that was treated with traditional instrumentation alone, and a total of 120 anteroposterior radiographs and fifty-five lateral radiographs were analyzed for the group that was treated with use of the custom tibial planing device. The mean coronal alignment of the tibial component was 89.5 degrees +/- 2.1 degrees in the group that was treated with traditional instrumentation alone and 89.6 degrees +/- 1.4 degrees in the group that was treated with use of the custom planing device. Although the mean coronal alignment was not significantly different, the number of outliers was substantially reduced when the custom planing device was used. All 120 components that had been aligned with use of the custom planing device were within 3 degrees of the target coronal alignment, compared with only eighty

  19. Excitation and damping of transversal oscillation in coronal loops by wake phenomena

    Directory of Open Access Journals (Sweden)

    A abedini

    2018-02-01

    Full Text Available Transversal oscillation of coronal loops that are interpreted as signatures of magneto hydrodynamics (MHD waves are observed frequently in active region corona loops. The amplitude of this oscillation has been found to be strongly attenuated. The damping of transverse oscillation may be produced by the dissipation mechanism and the wake of the traveling disturbance. The damping of transversal loop oscillations with wake phenomena is not related to any dissipation mechanism. Also, these kinds of coronal loop oscillations are not related to the kink mode, although this mode can be occurred after the attenuation process by the energy of the wave packet deposited in the loop.  In this paper the excitation and damping of transversal coronal loop oscillations with wake of traveling wave packet is discussed in detail, both theoretically and observationally. Here, the transversal coronal loop oscillations is modeled with a one dimensional simple line-tied. The dynamics of the loop and the coronal is governed by the Klein–Gordon differential equation. A localized disturbance that can be generated by nearby flare produces a perturbation that undergoes dispersion as it propagates toward the loop. As a consequence, the amplitudes of oscillates decay with time roughly t-1/2 at the external cutoff frequency. These observed data on 2016-Dec-4 by Atmospheric Imaging Assembly (AIA onboard Solar Dynamic Observatory (SDO observations data, consisting of 560 images with an interval of 24 seconds in the 171 A0 pass band is analyzed for evidence of excitation and damping of transverse oscillations of coronal loop that is situated near a flare. In this analyzed signatures of transverse oscillations that are damped rapidly were found, with periods in the range of P=18.5-23.85 minutes. Furthermore, oscillation of loop segments attenuate with time roughly as t-α that average values of α for 4 different loops change form 0.65-0.80. The magnitude values of α are in

  20. Supervivencia en pacientes con tuberculosis infectados por VIH. Estudio de los fallecimientos en los primeros nueve meses

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    Falqués Casanovas Meritxell

    1999-01-01

    Full Text Available FUNDAMENTO: En las personas con tuberculosis infectadas por el VIH, se ha observado una elevada letalidad durante las primeras semanas desde el inicio de la terapia antituberculosa. En el presente estudio se analiza la supervivencia de las mismas en el marco de un estudio de cohortes retrospectivo. MÉTODOS: Se incluyeron 1.135 individuos que correspondían a aquellos por el VIH mayores de quince años y residentes en Barcelona, registrados por el Programa de Prevención y Control de la Tuberculosis de Barcelona y que fueron diagnosticados entre 1988 y 1993. Las variables analizadas fueron edad, sexo, antecedentes de prisión, distrito municipal, grupo de riesgo, porcentaje de linfocitos T CD4+, prueba de la tuberculina, diagnóstico de sida (según criterio CDC-1987, patrón radiológico, bacteriología y localización anatómica de la tuberculosis. Se utilizó el método semiparamétrico de Cox, las curvas de Kaplan-Meier y la prueba de log-rank. RESULTADOS: La probabilidad de supervivencia a los nueve meses fue del 77%, con amplias variaciones en los diversos subgrupos. Las únicas variables significativas en el modelo multivariado de Cox fueron sida, porcentaje de linfocitos T CD4+ y su interacción. El riesgo de morir para un individuo sin SIDA y porcentaje de linfocitos T CD4+ inferior o igual al 14% fue 7.69 veces mayor que el riesgo de morir para un individuo sin SIDA y porcentaje de linfocitos T CD4+ superior al 14%. CONCLUSIONES: La supervivencia en las personas con tuberculosis infectadas por VIH es muy variable. Las que fallecieron a corto plazo fueron las diagnos