WorldWideScience

Sample records for astron

  1. Observatorio Astronómico Nacional, Colombia

    Science.gov (United States)

    Murdin, P.

    2000-11-01

    The Observatorio Astronómico Nacional (OAN) was founded by José Celestino Mutis in the framework of the `Expedicion Botanica' on 20 August 1803. His first astronomer was Francisco Jose de Caldas. By the turn of the century, Julio Garavito worked in celestial mechanics—a crater on the far side of the Moon bears his name....

  2. Observatorio Astronómico De Cantabria

    Science.gov (United States)

    Domínguez, R. M.; Carrera, F. J.

    The Astronomical Observatory of Cantabria is a center of the Consejería de Medio Ambiente del Gobierno de Cantabria managed by the Centro de Investigación del Medio Ambiente (CIMA), an autonomous organism which depends on such Consejería. The development of different activities of the Observatory is a joint collaboration between the University of Cantabria and the Agrupación Astronómica Cántabra (AstroCantabria). As part of the University of Cantabria, the Instituto de Física de Cantabria (IFCA, CSIC-UC) is in charge of the direction, management and coordination of scientific, observational, educational and outreach activities of the Observatory. AstroCantabria takes care of the outreach activities for the general public as well as the astronomical observations. In addition, it is responsible for the calibration and maintenance of the astronomical instrumentation of the Observatory. The Astronomical Observatory of Cantabria is located on the Southern edge of the Comunidad Autónoma de Cantabria, on the high plateau of La Lora (Valderredible county), at an altitude of 1,080m, with longitude 3∘ 56 ' 36' W and latitude 42∘ 46 ' 18' N. Rocamundo is the closest town. The Observatory aims to become a center of reference for scientific, observational, educational and public outreach activities in Cantabria. In the near future, an observational proposal system for outside users will be set in place.

  3. The RadioAstron Dedicated DiFX Distribution

    Directory of Open Access Journals (Sweden)

    Gabriele Bruni

    2016-10-01

    Full Text Available Distributed FX-architecture (DiFX is a software Very Long Baseline Interferometry (VLBI correlator currently adopted by several main correlation sites around the globe. After the launch of the RadioAstron Space-VLBI mission in 2011, an extension was necessary to handle processing of an orbiting antenna, to be correlated with supporting ground arrays. Here, we present a branch of the main DiFX distribution (2.4, uploaded on the publicly available repository during July 2016, that the Max Planck Institute for Radio Astronomy (MPIfR developed to process data of the three key active galactic nuclei (AGN-imaging RadioAstron science projects, as well as part of the AGN survey project, and General Observing Time (GOT projects proposed since Announcement of Opportunity 2 (AO-2, July 2014–July 2015. It can account for general relativistic correction of an orbiting antenna with variable position/velocity, providing a routine to convert the native RadioAstron Data Format (RDF format to the more common Mark5 B (M5B. The possibility of introducing a polynomial clock allows one to mitigate the effects of spacecraft acceleration terms in near-perigee observations. Additionally, since for the first time polarimetry on space-baselines is available thanks to RadioAstron, this DiFX branch allows one to include the spacecraft orientation information at the correlation stage, in order to perform proper polarization calibration during data reduction. Finally, a fringe-finding algorithm able to manage an arbitrarily large fringe-search window is included, allowing one to increase the search space normally adopted by common software packages like HOPS.

  4. Alfabetización astronómica

    Science.gov (United States)

    Tignanelli, H.

    A fines de 1991, en una revista de educación en ciencias, José L. Sérsic reflexionaba acerca de los problemas que enfrentaría la enseñanza de los conocimientos astronómicos en nuestro país, en los umbrales del Siglo XXI. Entonces postulaba como un objetivo mínimo, que los jóvenes deberían mostrar signos claros de que se hallan astronómicamente alfabetizados. Era el año en que se realizaba por primera vez una Asamblea General de I.A.U. en Buenos Aires, una oportunidad de singulares características para la comunidad astronómica local y, simultáneamente el comienzo de un cambio radical en la estructura del sistema educativo argentino. ?`Contempla ese cambio el objetivo que postulara Sérsic? ?`Estamos en condiciones de afirmar que estamos en camino de lograrlo? ?`Con qué parámetros?. Presentamos aquí un panorama general sobre algunas de las acciones realizadas en función de alcanzar esa alfabetización científica, analizando exclusivamente la actividad de enseñanza hasta el nivel universitario, sin detenernos en el mismo, ya que lo consideramos una instancia superior e independiente de aquella alfabetización. Tampoco nos referiremos a la tarea de difusión, divulgación o popularización de la Astronomía, ya que su condición de asistemática y subjetiva no es evaluable en términos de la formación integral de un individuo.

  5. Guía astronómica

    OpenAIRE

    Duque Escobar, Gonzalo

    2003-01-01

    Esta Guía Astronómica es una versión de mis conferencias en el Taller de Astronomía desde 1985 y en el curso de Contexto en Astronomía desde 2000, dos actividades ofrecidas por la Universidad Nacional de Colombia en Manizales, como espacios disponibles para la comunidad académica y para los aficionados a la astronomía. Por esa razón, este texto propio de la vida universitaria, ha evolucionado hasta encontrar el lenguaje sencillo y la medida adecuada en la extensión y profundidad de los tem...

  6. Aniversarios astronómicos en Cananea, Sonora

    Directory of Open Access Journals (Sweden)

    Raúl Pérez – Enríquez

    2013-06-01

    Full Text Available El 21 de marzo de 1913, en la ciudad de México, nació Guillermo Haro Barraza y el 27 de abril de 1988, se inauguró el Observatorio Astrofísico Guillermo Haro, en Cananea, Sonora. Estos dos muy importantes aniversarios astronómicos se conmemoraron el pasado 27 de abril. Aquí se da cuenta de la relevancia de ambos festejos, de la fructuosa vida del homenajeado y de las actividades desarrolladas ese día allá donde está instalada “Una mina de estrellas”.

  7. VizieR Online Data Catalog: Astron low resolution UV spectra (Boyarchuk+, 1994)

    Science.gov (United States)

    Boyarchuk, A. A.

    2017-05-01

    Astron was a Soviet spacecraft launched on 23 March 1983, and it was operational for eight years as the largest ultraviolet space telescope during its lifetime. Astron's payload consisted of an 80 cm ultraviolet telescope Spica and an X-ray spectroscope. We present 159 low resolution spectra of stars obtained during the Astron space mission (Tables 4, 5; hereafter table numbers in Boyarchuk et al. 1994 are given). Table 4 (observational log, logs.dat) contains data on 142 sessions for 90 stars (sorted in ascending order of RA), where SED was obtained by scanning method, and then data on 17 sessions for 15 stars (also sorted in ascending order of RA), where multicolor photometry was done. Kilpio et al. (2016, Baltic Astronomy 25, 23) presented results of the comparison of Astron data to the modern UV stellar data, discussed Astron precision and accuracy, and made some conclusions on potential application areas of these data. Also 34 sessions of observations of 27 stellar systems (galaxies and globular clusters) are presented. Observational log was published in Table 10 and data were published in Table 11, respectively. Also 16 sessions of observations of 12 nebulae (Table 12 for observational log and Table 13 for data themselves) are presented. Background radiation intensity data (Table 14) are presented in Table 15. At last, data on comets are presented in different forms. We draw your attention that observational data for stars, stellar systems, nebulae and comets are expressed in log [erg/s/cm^2/A], while for comets data 10E-13 erg/s/cm^2/A units are used, hydroxyl band photometric data for comets are expressed in log [erg/s/cm^2], and for the background data it is radiation intensity expressed in log [erg/s/cm^2/A/sr]. Scanned (PDF version of) Boyarchuk et al. (1994) book is available at http://www.inasan.ru/~astron/astron.pdf (12 data files).

  8. Gravitational Redshift Experiment with the Space Radio Telescope RadioAstron

    CERN Document Server

    Litvinov, D; Belousov, K; Bietenholz, M; Biriukov, A; Fionov, A; Gusev, A; Kauts, V; Kovalenko, A; Kulagin, V; Poraiko, N; Rudenko, V

    2015-01-01

    A unique test of general relativity is possible with the space radio telescope RadioAstron. The ultra-stable on-board hydrogen maser frequency standard and the highly eccentric orbit make RadioAstron an ideal instrument for probing the gravitational redshift effect. Large gravitational potential variation, occurring on the time scale of $\\sim$24 hr, causes large variation of the on-board H-maser clock rate, which can be detected via comparison with frequency standards installed at various ground radio astronomical observatories. The experiment requires specific on-board hardware operating modes and support from ground radio telescopes capable of tracking the spacecraft continuously and equipped with 8.4 or 15 GHz receivers. Our preliminary estimates show that $\\sim$30 hr of the space radio telescope's observational time are required to reach $\\sim 2\\times10^{-5}$ accuracy in the test, which would constitute a factor of 10 improvement over the currently achieved best result.

  9. VIII Olimpíada Brasileira de Astronomia e Astronáutica

    Science.gov (United States)

    Garcia Canalle, João Batista; Villas da Rocha, Jaime Fernando; Wuensche de Souza, Carlos Alexandre; Pereira Ortiz, Roberto; Aguilera, Nuricel Villalonga; Padilha, Maria De Fátima Catta Preta; Pessoa Filho, José Bezerra; Soares Rodrigues, Ivette Maria

    2007-07-01

    Neste trabalho apresentamos as motivações pelas quais organizamos, em conjunto, pela primeira vez, a Olimpíada Brasileira de Astronomia incluindo a Astronáutica, em colaboração com a Agência Espacial Brasileira. Esta ampliação contribuiu para atrair ainda mais alunos, professores, escolas e patrocinadores para participarem desta Olimpíada. Em 2005 participaram da VIII Olimpíada Brasileira de Astronomia e Astronáutica (VIII OBA) 187.726 alunos distribuídos por 3.229 escolas, pertencentes a todos os estados brasileiros, incluindo o Distrito Federal. O crescimento em número de alunos participantes foi 52,4% maior do que em 2004. Em abril de 2005 organizamos, em Itapecerica da Serra, SP, um curso para os 50 alunos previamente selecionados e participantes da VII OBA e ao final selecionamos, dentre eles, uma equipe de 5 alunos, os quais representaram o Brasil na X Olimpíada Internacional de Astronomia, na China, em outubro de 2005. Ganhamos, pela primeira vez, uma medalha de ouro naquele evento. Em Agosto de 2005, organizamos a VIII Escola de Agosto para 50 alunos e respectivos professores, em Águas de Lindóia, SP, juntamente com a XXXI reunião anual da Sociedade Astronômica Brasileira (SAB). Em novembro de 2005 realizamos a I Jornada Espacial, em São José dos Campos, com 22 alunos e 22 professores selecionados dentre os participantes que melhores resultados obtiveram nas questões de Astronáutica da VIII OBA. Neste trabalho detalhamos os resultados da VIII OBA bem como as ações subseqüentes.

  10. Practical Astronomical Activities during Daytime. (Spanish Title: Actividades Astronómicas Prácticas Diurnas.) Atividades Astronômicas Práticas Diurnas

    Science.gov (United States)

    Jackson, Eric

    2009-12-01

    These daytime astronomy activities arose from research done in New Zealand by a group of teachers and astronomers into the problems of teaching astronomy. This showed that it was generally regarded as a difficult subject to take, traditionally relying on books, films and models. The fortunate may have had a visit to an observatory or planetarium, the adventurous may have attempted an outdoor evening viewing session, which sometimes had weather-related difficulties. The problem of not having many 'hands-on' activities, the feelings of inadequate knowledge, the felt need for astronomical equipment and expertise become too daunting for many teachers to do the subject justice. If astronomy was to be taught then a way around these difficulties needed to be found. Our group, working with teachers and children using the constructivism teaching approach, found that the principles of astronomy could be discovered during the day when the students are at school. Working co-operatively they measured and recorded observations of their shadows caused by the motions and interactions of the nearest star, the Sun (Sol), and our planet, Earth. Because children were involved so personally they were much more interested in the results of the study. Astronomy became enthralling and challenging for both teacher and class after applying their daytime experiences to night time viewing at home and reporting back to class. Estas actividades astronómicas diurnas surgieron de una investigación hecha en NuevaZelandia por un grupo de maestros y astrónomos sobre los problemas de la enseñanza de la Astronomía. Este trabajo mostró que la Astronomía es generalmente considerada una disciplina difícil de enseñar, y tradicionalmente basada en libros, filmes y modelos. Los más afortunados pueden haber efectuado alguna visita a un observatorio o planetario, y los más aventajados pueden tal vez haber intentado una sesión de observación nocturna, las cuales sufren a veces de dificultades

  11. RadioAstron and millimetron space observatories: Multiverse models and the search for life

    Science.gov (United States)

    Kardashev, N. S.

    2017-04-01

    The transition from the radio to the millimeter and submillimeter ranges is very promising for studies of galactic nuclei, as well as detailed studies of processes related to supermassive black holes, wormholes, and possible manifestations of multi-element Universe (Multiverse) models. This is shown by observations with the largest interferometer available—RadioAstron observatory—that will be used for the scientific program forMillimetron observatory. Observations have also shown the promise of this range for studies of the formation and evolution of planetary systems and searches for manifestations of intelligent life. This is caused by the requirements to use a large amount of condensedmatter and energy in large-scale technological activities. This range can also be used efficiently in the organisation of optimal channels for the transmission of information.

  12. Plataforma de objetos web para el control remoto del observatorio astronómico Francisco Sánchez

    OpenAIRE

    Martínez Villacampa, Javier

    2017-01-01

    El observatorio astronómico Francisco Sánchez está compuesto por diversos elementos controlables a través de varios dispositivos electrónicos. Dichos dispositivos se encuentran conectados en red e implementan cada uno un protocolo adhoc de comunicación sobre HTTP. Cada protocolo permite controlar de forma remota su dispositivo correspondiente, de forma que dichos dispositivos podrían considerarse como objetos del Internet de las cosas. Este proyecto tiene como objetivo desar...

  13. Determinación astronómica de la Desviación de la Vertical

    Science.gov (United States)

    Pacheco, A. M.; Podestá, R. C.

    A partir de las coordenadas astronómicas de Latitud y Longitud determinadas en la falla geológica de Nikizanga ubicada en las serranías de Pie de Palo, y, en base a un Punto Datum de referencia, se desarrolla la metodología para la determinación de la Desviación de la Vertical, que comprende la reducción de las observaciones astronómicas, transformaciones de coordenadas, aplicación de correcciones y el cálculo definitivo de los valores angulares de la Vertical. Estos estudios se iniciaron a sugerencia del Servicio Internacional de Latitud, International Polar Motion Service (IPMS), con el objeto de obtener en determinados puntos de la Tierra la Desviación de la Vertical y su variación, dentro de la nueva disciplina denominada Astrogeodinámica, con la idea de correlacionar estas variaciones con la predicción de grandes sismos.

  14. PKS 1954-388: RadioAstron Detection on 80,000 km Baselines and Multiwavelength Observations

    Science.gov (United States)

    Edwards, P. G.; Kovalev, Y. Y.; Ojha, R.; An, H.; Bignall, H.; Carpenter, B.; Hovatta, T.; Stevens, J.; Voytsik, P.; Andrianov, A. S.; Dutka, M.; Hase, H.; Horiuchi, S.; Jauncey, D. L.; Kadler, M.; Lisakov, M.; Lovell, J. E. J.; McCallum, J.; Müller, C.; Phillips, C.; Plötz, C.; Quick, J.; Reynolds, C.; Schulz, R.; Sokolovsky, K. V.; Tzioumis, A. K.; Zuga, V.

    2017-04-01

    We present results from a multiwavelength study of the blazar PKS 1954-388 at radio, UV, X-ray, and gamma-ray energies. A RadioAstron observation at 1.66 GHz in June 2012 resulted in the detection of interferometric fringes on baselines of 6.2 Earth-diameters. This suggests a source frame brightness temperature of greater than 2 × 1012 K, well in excess of both equipartition and inverse Compton limits and implying the existence of Doppler boosting in the core. An 8.4-GHz TANAMI VLBI image, made less than a month after the RadioAstron observations, is consistent with a previously reported superluminal motion for a jet component. Flux density monitoring with the Australia Telescope Compact Array confirms previous evidence for long-term variability that increases with observing frequency. A search for more rapid variability revealed no evidence for significant day-scale flux density variation. The ATCA light-curve reveals a strong radio flare beginning in late 2013, which peaks higher, and earlier, at higher frequencies. Comparison with the Fermi gamma-ray light-curve indicates this followed 9 months after the start of a prolonged gamma-ray high-state-a radio lag comparable to that seen in other blazars. The multiwavelength data are combined to derive a Spectral Energy Distribution, which is fitted by a one-zone synchrotron-self-Compton (SSC) model with the addition of external Compton (EC) emission.

  15. "Los costarricenses no han dejado de admirar las magnificencias del cielo": La evolución de las ideas astronómicas en Costa Rica (1814 - 1910.

    Directory of Open Access Journals (Sweden)

    Ronald Eduardo Díaz Bolaños

    2011-08-01

    Full Text Available El trabajo analiza cómo a lo largo del siglo XIX, se produjo un gran desarrollo de las ideas astronómicas en Costa Rica, hechas por las investigaciones de científicos locales y extranjeros. En concreto el trabajo procura analizar los procesos que promovieron el desarrollo de esas ideas astronómicas en el país, con la apertura de la primera casa de estudios superiores (1814 hasta el desenlace de la mayor polémica científica relacionada con esta ciencia en por el paso del cometa Halley (1910.

  16. Centro astronómico de Calar-Alto Almería – España

    Directory of Open Access Journals (Sweden)

    Margarit, Salvador

    1980-08-01

    Full Text Available The Basic Agreement of Cooperation in Scientific Research and Technological development signed by the Spanish and West German governments in 1970, served as a framework for the agreement signed in 1972 by the National Astronomical Commission and the Max-Planck Society, for the setting up of the «Spanish-German Astronomical Centre». Construction work was started in 1973 on the Calar-Alto (2,168 m, the highest point in the Sierra de los Filabres in the province of Almería. At present the last of the domed buildings, which is intented to accommodate a 3.5 m diameter Telescope and should go into operation in 1983, is at the completion stage. By this date all work will have been completed, with four domed buildings for telescopes of different sizes and the buildings for laboratory, living quarters, services and workshops needed for the use of the scientific instruments. The 1.52 m diameter National Astronomical Observatory telescope has been installed in a separate building beside the infrastructure of the Spanish-German Astronomical Centre.

    El Convenio Básico de Cooperación en la Investigación Científica y en el Desarrollo tecnológico suscrito entre los gobiernos de España y de la República Federal de Alemania en 1970, sirvió de marco para el acuerdo firmado en 1972 entre la Comisión Nacional de Astronomía y la Sociedad Max-Planck, para el establecimiento del «Centro Astronómico» Hispano-Alemán. En 1973 se iniciaron los trabajos de Obras en Calar-Alto (2.168 m cota máxima de la Sierra de los Filabres en la provincia de Almena. Actualmente se halla en fase de terminación el último de los edificios de Cúpula destinado a albergar un Telescopio de 3,5 m de diámetro y cuya puesta en servicio se prevé en 1983. Para entonces quedará culminada la realización completa con cuatro edificios de Cúpula para telescopios de diferentes tamaños y las edificaciones destinadas a laboratorio, residencia, viviendas, servicios y

  17. El «Plan de las inmediaciones» del Observatorio Astronómico: Un Proyecto desaparecido de Juan de Villanueva

    Directory of Open Access Journals (Sweden)

    Laca Menéndez de Luarca, Luis Ramón

    1999-09-01

    Full Text Available This paper reconstructs the "plan de las inmediaciones" ("project for the surroundings" hypothetically composed by Juan de Villanueva for Madrid Observatorio Astronómico, today disappeared. The data emanated from the drawing dedied to the Observatorio by Isidro Velazquez, Villanueva's best disciple, as well as from the parcel, allow to draw the perfect integration between the building and the surrounding landscape. Because of a number of circumstances two important elements are losten, the original access building and the great 25 feet telescope. Nevertheless, the restoration of the scene conceived by Villanueva, and later drawn by Velazquez, is still perfectly possible.No disponible

  18. Análise dos Conceitos Astronômicos Apresentados por Professores de Algumas Escolas Estaduais Brasileiras

    Science.gov (United States)

    Voelzke, Marcos Rincon; Gonzaga, Edson Pereira

    2011-12-01

    A razão para o desenvolvimento deste trabalho baseia-se no fato de que muitos professores da Educação Básica (EB) não lidam com conceitos relacionados à astronomia, e quando o fazem eles simplesmente seguem livros didáticos que podem conter erros conceituais. Como é de conhecimento geral a astronomia é um dos conteúdos a serem ensinados na EB fazendo parte dos Parâmetros Curriculares Nacionais e das Propostas Curriculares do Estado de São Paulo, mas é um fato, que vários pesquisadores apontam, a existência de muitos problemas no ensino da astronomia. Com o propósito de minimizar algumas dessas deficiências foi realizado um trabalho de pesquisa com a utilização de questionários pré e pós pesquisa, para tanto foi desenvolvido um Curso de Extensão Universitária para professores da Diretoria de Ensino Regional (DE) que abrange Mauá, Ribeirão Pires e Rio Grande da Serra (no Estado de São Paulo) com os seguintes objetivos: levantar concepções alternativas; subsidiar os professores por meio de palestras, debates e workshops, e verificar o sucesso da aprendizagem após o curso, adotando-se como referência, para a análise dos resultados, os dicionários de Língua Portuguesa (FERREIRA, 2004) e Enciclopédico de Astronomia e Astronáutica (MOURĀO, 1995). Portanto, dezesseis questões foram aplicadas antes e após o curso, assim pode-se verificar após a pesquisa que 100,0% dos professores sabiam os nomes das fases da Lua, 97,0% entenderam que o Sistema Solar é composto por oito planetas, 78,1% foram capazes de explicar como ocorre um eclipse lunar, um eclipse solar e um solstício, 72,7% sabiam como explicar a ocorrência das estações do ano; 64,5% explicaram corretamente a ocorrência do equinócio, 89,7% foram capazes de definir adequadamente o termo cometa; 63,6% definiram asteróide, 54,5% meteoro, 58,1% galáxia, e 42,4% planeta. Os resultados obtidos indicam uma aprendizagem significativa por parte dos participantes.

  19. Percepção Astronômica de Alunos do Ensino Médio da Rede Estadual de São Paulo

    Science.gov (United States)

    de Oliveira, E. F.; Voelzke, M. R.; Amaral, L. H.

    2005-08-01

    Embora a astronomia seja uma das ciências mais antigas da humanidade e muitos dos conceitos astronômicos serem populares, principalmente nesta época de alta globalização do conhecimento por intermédio de eficientes meios de comunicação e de obtenção da informação, notadamente através da internet, observa-se que uma parcela significativa dos estudantes encontra-se à margem dessas informações. O presente trabalho visa analisar o nível de conhecimento básico dos alunos de Ensino Médio da rede estadual da cidade de Suzano quanto aos fenômenos astronômicos que os rodeiam, tais como a sucessão dos dias e das estações do ano, além de questioná-los sobre fatos genéricos tais como: quais são os astros que se encontram mais próximos do planeta Terra, o que vem a ser o Sol, o Big Bang, um ano-luz, uma estrela cadente, a estrela de Bélem e o que ocasionou a extinção dos dinossauros. Para tanto foi elaborado um formulário constando de questões de múltipla escolha, o qual foi aplicado no primeiro colegial noturno da Escola Estadual Batista Renzi. Num espaço amostral de 34 alunos constatou-se que apenas 29,4% compreendiam a sucessão dos dias da semana, que apenas 20,6% explicaram corretamente as estações do ano, que apenas 20,6% tinham idéia de quais são os objetos celestes mais próximos da Terra, em contraposição 67,6% sabiam classificar corretamente o Sol como estrela, 55,9% relacionavam o Big Bang à origem do universo, apenas 20,6% identificavam um ano-luz como unidade de distância, 32,4% reconheciam uma estrela cadente como meteoro, 41,2% consideravam a estrela de Belém como um cometa e 50,0% explicaram corretamente a extinção dos dinossauros. A presente análise será expandida para as demais classes de primeiro colegial, não somente do período noturno, mas também do diurno da Escola Estadual Batista Renzi, bem como o formulário será devidamente ampliado. Já nesta primeira fase nota-se claramente o pequeno discernimento

  20. A Influência da Escola e da Mídia na Obtenção dos Conhecimentos Astronômicos

    Science.gov (United States)

    da Cunha, W. S.; Voelzke, M. R.; Amaral, L. H.

    2006-08-01

    O universo em que vivemos possui segredos jamais imaginados pelo homem, fruto da pequena proporção que ocupamos diante de um cosmos infinito. A astronomia funciona como um instrumento que sacia a sede humana em desvendar esses segredos, estudando as galáxias, quasares, pulsares além da existência de todos os elementos que preenchem o espaço cósmico, o vácuo, não mais vazio como se pensou em outros tempos. A mídia explora esse campo de forma mística e também científica. A difusão adequada e dentro dos padrões educacionais vigentes, de conceitos astronômicos, se faz necessária, devido sua presença nos conteúdos escolares, centros de ciência e na mídia, de modo geral. A reforma do Currículo Básico da Escola Pública da maioria dos Estados brasileiros introduziu conceitos astronômicos desde a pré-escola até o Ensino Médio. Num estudo realizado com 1.032 alunos do Ensino Médio de seis escolas estaduais, revelou-se através da aplicação de um questionário que abordava conheciment os básicos em astronomia, como estes foram adquiridos e qual era a infra-estrutura oferecida pela escola: para 66,2% dos entrevistados o professor já fez alguma apresentação a respeito de astronomia. O presente estudo revelou também que 44,5% dos alunos entrevistados adquiriram seus conhecimentos astronômicos na escola, 28,1% através da televisão e 27,4% afirmaram que seus conhecimentos foram obtidos através de outros tipos de mídia (internet, filmes e revistas). Embora o estudo revele claramente que há certo equilíbrio na forma em que os alunos obtiveram seus conhecimentos astronômicos, a mídia ainda explora e muitas vezes desperta o interesse pela astronomia com assuntos que não fazem parte de nosso cotidiano como, por exemplo, o homem na Lua, os projetos espaciais e a primeira viagem de um astronauta brasileiro no espaço. Porém, em certos casos, a mídia pode promover conhecimentos incompletos ou mesmo equivocados sobre os conceitos que envolvam

  1. RadioAstron space VLBI imaging of polarized radio emission in the high-redshift quasar 0642+449 at 1.6 GHz

    Science.gov (United States)

    Lobanov, A. P.; Gómez, J. L.; Bruni, G.; Kovalev, Y. Y.; Anderson, J.; Bach, U.; Kraus, A.; Zensus, J. A.; Lisakov, M. M.; Sokolovsky, K. V.; Voytsik, P. A.

    2015-11-01

    Context. Polarization of radio emission in extragalactic jets at a sub-milliarcsecond angular resolution holds important clues for understanding the structure of the magnetic field in the inner regions of the jets and in close vicinity of the supermassive black holes in the centers of active galaxies. Aims: Space VLBI observations provide a unique tool for polarimetric imaging at a sub-milliarcsecond angular resolution and studying the properties of magnetic field in active galactic nuclei on scales of less than 104 gravitational radii. Methods: A space VLBI observation of high-redshift quasar TXS 0642+449 (OH 471), made at a wavelength of 18 cm (frequency of 1.6 GHz) as part of the early science programme (ESP) of the RadioAstron mission, is used here to test the polarimetric performance of the orbiting Space Radio Telescope (SRT) employed by the mission, to establish a methodology for making full Stokes polarimetry with space VLBI at 1.6 GHz, and to study the polarized emission in the target object on sub-milliarcsecond scales. Results: Polarization leakage of the SRT at 18 cm is found to be within 9% in amplitude, demonstrating the feasibility of high fidelity polarization imaging with RadioAstron at this wavelength. A polarimetric image of 0642+449 with a resolution of 0.8 mas (signifying an ~4 times improvement over ground VLBI observations at the same wavelength) is obtained. The image shows a compact core-jet structure with low (≈2%) polarization and predominantly transverse magnetic field in the nuclear region. The VLBI data also uncover a complex structure of the nuclear region, with two prominent features possibly corresponding to the jet base and a strong recollimation shock. The maximum brightness temperature at the jet base can be as high as 4 × 1013 K.

  2. Como os Alunos do Ensino Médio da Rede Estadual de São Paulo obtém Conhecimentos Astronômicos?

    Science.gov (United States)

    da Cunha, W. S.; Voelzke, M. R.; Amaral, L. H.

    2005-08-01

    Atualmente vivencia-se um mundo globalizado onde os computadores e a internet permitiram um acesso rápido e seguro a todo tipo de informação e conhecimento. O presente trabalho visa analisar a maneira pela qual alunos de segundo grau da rede estadual da cidade de São Paulo obtiveram, caso tenham, conhecimentos básicos de astronomia quanto aos fenômenos celestes que os rodeiam, tais como a sucessão dos dias e das estações do ano, além de questioná~los sobre fatos genéricos tais como: o que vem a ser o Sol, o Big Bang, o que ocasionou a extinção dos dinossauros. Para tanto foi elaborado um formulário constando de questões de múltipla escolha, o qual foi aplicado no primeiro colegial diurno da Escola Estadual Guilherme de Almeida. Num espaço amostral de 44 alunos constatou-se que 41% dos alunos adquiriram seus conhecimentos astronômicos na escola e 59% através da mídia em geral. Neste mesmo espaço amostral apenas 11% dos alunos usaram computadores na escola, 41% na residência, 5% no trabalho e 43% não utilizaram. O presente estudo revelou também que para 50% dos alunos o professor jamais utilizou um programa de computador a respeito de astronomia ou fez alguma apresentação sobre o tema. Embora em sua fase inicial este estudo revela claramente que a maioria dos alunos não obtém na escola seus conhecimentos astronômicos, estes provém de fontes não especificamente didático-pedagógicas tais como filmes e revistas populares que não raramente geram conhecimentos incompletos e em muitos casos inclusive falhos.

  3. Improvement of the orbit of the Spektr-R spacecraft in the RadioAstron mission and required conditions for improvement using a Kalman filter

    Science.gov (United States)

    Zhamkov, A. S.; Zharov, V. E.

    2017-05-01

    This paper is concerned with improvement of the state vector of the Spektr-R spacecraft of the RadioAstron mission. The state vector includes three coordinates of the position of the spacecraft and three components of its velocity in the Geocentric Celestial Reference System. Improvement of the orbit of the spacecraft is understood as improvement of the state vector. The results are compared with the original orbits determined at the Keldysh Institute of Applied Mathematics (IAM). The paper considers both using the Kalman filter based on a single set of radio-range and Doppler data from ground-based stations and the analysis of conditions that will lead to improvement of the orbit. It has been shown that using three ground-based stations that perform simultaneous measurements the problem is solved completely, even when a poor initial approximation is used. Based on the results, a list of requirements is obtained that will provide more accurate information on the orbit of the Spektr-R spacecraft.

  4. Google Sky y los estándares de catalogación: un ejemplo de divergencia entre la información astronómica existente y la que se puede describir

    Directory of Open Access Journals (Sweden)

    Alonso-Lifante, M. Pilar

    2013-12-01

    Full Text Available A survey has been carried out on the astronomical information supplied by Google Sky and the information which can be described using the standards MARC21, ISBD consolidated edition, and RDA. The main goal of the study is to show that some astronomical and astrophysical information is still not taken into account in describing different astronomical resources as well as cartographic material. This information could eventually be incorporated as description fields of the aforementioned cataloguing rules. Such fields would allow us to carry out a much more complete and adequate description of these astronomical resources. We have focused on celestial objects appearing in astronomical images which can be found in astronomical archives and libraries. First a brief survey of astronomical information supplied by Google Sky and its linked databases, SIMBAD and NED is performed. Subsequently, we show how the existing description fields describe celestial cartographic materials, and finally we present a new proposal consisting of the desirable minimum parameters which could be included in bibliographic records.Se realiza una revisión tanto de la información astronómica que ofrece Google Sky como la que permiten describir MARC21, ISBD consolidada y RDA, para demostrar que no se han contemplado hasta el momento determinados parámetros astronómicos y astrofísicos, susceptibles de convertirse en futuros campos de descripción de estos estándares. Dichos campos permitirán realizar descripciones mucho más completas y adecuadas de diferentes recursos astronómicos como material cartográfico. En concreto, se analizan exclusivamente aquellos objetos celestes contenidos en imágenes astrofotográficas que pueden encontrarse en archivos y bibliotecas astronómicas. Para ello, primero se realiza una síntesis de la información astronómica que ofrecen Google Sky y las bases de datos a las que enlaza, SIMBAD y NED. Posteriormente se indican los campos de

  5. Qual o Papel da Escola e da Mídia na Obtenção dos Conhecimentos Astronômicos?

    Science.gov (United States)

    da Cunha, W. S.; Voelzke, M. R.; Amaral, L. H.

    2007-08-01

    É amplamente reconhecido que as pessoas em geral têm grande fascínio e interesse pela Astronomia. Por outro lado, o conteúdo dessa área incluído no ensino formal está longe de ser abrangente e suficiente para suprir a demanda. Esse interesse permite aperfeiçoar a divulgação e o ensino não formal de Astronomia através da mídia aliando a adequação do conteúdo à expectativa das pessoas. A reforma do Currículo Básico da Escola Pública da maioria dos Estados brasileiros tem introduzido Astronomia desde a pré-escola até o Ensino Médio. Num estudo realizado com 1180 alunos do Ensino Médio de seis escolas estaduais, revelou-se através da aplicação de um formulário contendo questões que abordavam conhecimentos básicos em Astronomia, como foram adquiridos tais conhecimentos e à infra-estrutura da escola. Para 66,1% dos entrevistados o professor já fez alguma apresentação a respeito de Astronomia. O presente estudo revelou também que 54,4% dos alunos entrevistados adquiriram seus conhecimentos astronômicos na escola, 18,4% através da televisão e 27,1% afirmaram que seus conhecimentos foram obtidos através de outros tipos de mídia (internet, livros didáticos, filmes e revistas). Embora o estudo revele claramente que há certo equilíbrio no meio em que os alunos obtiveram seus conhecimentos astronômicos, a mídia busca não somente sua difusão, mas a disponibilização desse conhecimento de maneira correta, que às vezes, não é atingido, apresentando conceitos sem fundamentação e incorretos. Por outro lado, no dia-a-dia escolar, é comum encontrar professores que vêm para as aulas com concepções prévias, que podem diferir substancialmente das idéias a serem ensinadas, dificultando o aprendizado de futuros conceitos científicos. Uma avaliação criteriosa, avaliando as dificuldades dos professores em determinar o sentido correto dos conceitos e observando a metodologia que utilizam no ensino, poderá proporcionar uma melhor

  6. Mediciones de irradiancia solar y capa de ozono durante el eclipse de Sol de 1994 en el Observatorio Astronómico de Rosario, Argentina

    Science.gov (United States)

    Piacentini, R. D.; Micheletti, M. I.

    We show results of measurements made during the Sun's eclipse of November 3, 1994, in Observatorio Astronómico de Rosario (32o 57' S, 60o 37' W, 25 m a.s.l.). The eclipse begin at 8:41 local hour, reached its maximum with 77% of the surface covered at 9:51 and finished at 11:04. The direct solar irradiance of 300 nm and 313 nm were able to be measured, due to the fact that during the whole period the sky remained completed uncovered (zero percent cloudiness). The measurements were made with the portable ozonometer developed by Tocho and co-workers. They show the characterictic decrease due to the occultation of the source, which is approximately proportional to the surface's diminution. When crossing the earth's atmosphere to arrive to the observation point, these irradiances are affected mainly by the ozone layer, specially the irradiance at lower wavelength, what let it to determine by comparison the thickness of this layer. The total ozone thickness distributed between the troposphere and the stratosphere shows an oscillation, whose amplitude, since the occurence of the maximum of occulation, has a mean value of 4%, and whose period is of approximately 2100 seconds, being both numbers considerably larger than the ones registred by Mims III y Mims (Geophysical Research Letters, 20, 367, 1993) during the eclipse of July 11, 1991 and by Tocho, Da Silva y Rivas (XVIII Quadriennial Ozone Symposiom, Italy, September, 1996) during the same eclipse analyzed in the present work, but observed in Salta. As complementary results, we measured the global irradiance and the ambient temperature during this astronomical event.

  7. A Reappraising of Cosmography: the Interface Between Astronomical and Geographic Studies. (Breton Title: Releitura do Conceito de Cosmografia: a Interface Entre os Estudos Astronômicos e Geográficos.) Una Relectura del Concepto de Cosmografía: la Interfase Entre los Estudios Astronómicos y Geográficos

    Science.gov (United States)

    Azevedo Sobreira, Paulo Henrique

    2012-12-01

    The concept of "Cosmography" is in disuse since the 80s of the last century, but the astronomical themes previously discussed in the school subjects of Geography and Cosmography remain in current textbooks. The use of term "Cosmography" was rescued in this research, and the study of its re-signification prompted the appearance of the term Geographic Cosmography. The Geographic Cosmography is a field of studies of the Geography, whose set of knowledge and skills is predominantly scholar. It studies the interface between terrestrial and celestial knowledge, and assigns a geographic significance to them. It examines human and natural relationships with Sidereal Space and its consequences for society and nature. O conceito de "Cosmografia" está em desuso desde os anos 80 do século XX, mas os temas astronômicos anteriormente abordados nas disciplinas escolares de Cosmografia e de Geografia permanecem nos atuais livros didáticos. O uso do termo "Cosmografia" foi resgatado nesta pesquisa e o estudo de sua ressignificação proporcionou o surgimento do termo Cosmografia Geográfica. A Cosmografia Geográfica é um campo de estudos da Geografia, cujo conjunto de conhecimentos e habilidades é predominantemente escolar. Estuda a interface entre os conhecimentos terrestres e os celestes e lhes atribui significância geográfica. Analisa as relações humanas e naturais com o Espaço Sideral e suas consequências para a sociedade e a natureza. Aunque el concepto de "Cosmografía" no se usa desde la década de los '80 del siglo pasado, los temas astronómicos que se enseñaban anteriormente en las asignaturas escolares de Cosmografía y de Geografía permanecen en los actuales libros didácticos. El uso del término "Cosmografía" fue rescatado en esta investigación y el estudio de su resignificación proporcionó el surgimiento del término Cosmografía Geográfica. La Cosmografía Geográfica es un campo de estudio de la Geografía, donde el conjunto de conocimientos y

  8. Tipología de recursos astronómicos históricos y fondos documentales en las cartotecas españolas: estado de la cuestión

    Directory of Open Access Journals (Sweden)

    Alonso-Lifante, M. Pilar

    2015-09-01

    Full Text Available The state of the art about a type of specialised resource with great historical and scientific value is presented: the astronomical documentation. First of all, the main types of astronomical resources are defined focusing on their historical evolution. Secondly, the result of a survey carried out between April and May 2014 about the astronomical collections in Spanish map libraries and archives is shown taking as a reference the IBERCARTO directory of 2012. Conclusions show that almost half of queried libraries and archives map have these type of documents, but disseminated in different collections. Moreover, around 70% of the institutions have catalogued all of their astronomical documentation and have used the classical encoding (MARC 21 and cataloguing standards (ISBD and ISAD(G, although recent studies have shown that these standards are not the most suitable ones to describe it. Hence, a satisfactory scientific information retrieval is not achieved.Se presenta el estado de la cuestión de un tipo de recurso especializado de gran valor histórico y científico: la documentación astronómica. Para ello, en primer lugar se definen los principales tipos de recursos astronómicos existentes señalando su evolución histórica. En segundo lugar se presentan los resultados de un estudio, realizado entre abril y mayo de 2014, sobre los fondos astronómicos existentes en cartotecas españolas, tomando como referencia el directorio de IBERCARTO de 2012. Las conclusiones indican que casi la mitad de las cartotecas encuestadas conservan documentos de este tipo, encontrándose dispersos en diferentes colecciones. Además, en torno al 70% de las instituciones tienen catalogada toda su documentación astronómica, descrita con los estándares clásicos de codificación (MARC 21 y catalogación (ISBD e ISAD(G, aunque recientes estudios han puesto de manifiesto que estos estándares no son los más adecuados para describirla, por lo que actualmente no se

  9. NASA's Astronant Family Support Office

    Science.gov (United States)

    Beven, Gary; Curtis, Kelly D.; Holland, Al W.; Sipes, Walter; VanderArk, Steve

    2014-01-01

    During the NASA-Mir program of the 1990s and due to the challenges inherent in the International Space Station training schedule and operations tempo, it was clear that a special focus on supporting families was a key to overall mission success for the ISS crewmembers pre-, in- and post-flight. To that end, in January 2001 the first Family Services Coordinator was hired by the Behavioral Health and Performance group at NASA JSC and matrixed from Medical Operations into the Astronaut Office's organization. The initial roles and responsibilities were driven by critical needs, including facilitating family communication during training deployments, providing mission-specific and other relevant trainings for spouses, serving as liaison for families with NASA organizations such as Medical Operations, NASA management and the Astronaut Office, and providing assistance to ensure success of an Astronaut Spouses Group. The role of the Family Support Office (FSO) has modified as the ISS Program matured and the needs of families changed. The FSO is currently an integral part of the Astronaut Office's ISS Operations Branch. It still serves the critical function of providing information to families, as well as being the primary contact for US and international partner families with resources at JSC. Since crews launch and return on Russian vehicles, the FSO has the added responsibility for coordinating with Flight Crew Operations, the families, and their guests for Soyuz launches, landings, and Direct Return to Houston post-flight. This presentation will provide a summary of the family support services provided for astronauts, and how they have changed with the Program and families the FSO serves. Considerations for future FSO services will be discussed briefly as NASA proposes one year missions and beyond ISS missions. Learning Objective: 1) Obtain an understanding of the reasons a Family Support Office was important for NASA. 2) Become familiar with the services provided for astronauts and their families and how they changed with the Program and family needs.

  10. The Meanings of Astronomical Observation: An Analysis on the Basis of Relationship with Knowledge. (Spanish Title: Los Sentidos de la Observación Astronómica: un Análisis sobre la Base de la Relación con el Saber.) Os Sentidos da Observação Astronômica: Uma Análise com Base na Relação com o Saber

    Science.gov (United States)

    Klein, Alberto Eduardo; de Mello Arruda, Sergio; Meneghello Passos, Marinez; Vinicius Domenes Zapparoli, Ferdinando

    2010-12-01

    This article presents results of a research which aimed to understand the meanings that people construct for astronomical observation. The subjects, students and school teachers, initially received some instruction on how to view astronomical objects through the telescope. After the observation was realized, they were interviewed. The data analysis allowed the creation of 12 categories, later interpreted on the basis of relationship with knowledge (relation to the world, with himself and with others), as presented by Bernard Charlot. Este artículo presenta los resultados de una investigación que tuvo como objetivo comprender los sentidos que las personas construyen para la observación astronómica. Los sujetos, los estudiantes y maestros de escuela, recibieron inicialmente algunas instrucciones sobre cómo ver los objetos astronómicos a través del telescopio. Al término de la observación, fueron entrevistados. El análisis de datos permitió la creación de 12 categorías que más tarde fueron interpretadas sobre la base de la relación con el conocimiento (relación con el mundo, consigo mismo y con los demás), tal como presentado por Bernard Charlot. Este artigo apresenta resultados de uma pesquisa que objetivou entender quais os sentidos que as pessoas constroem para a observação astronômica. Os sujeitos da pesquisa, estudantes e professores do ensino médio, receberam inicialmente alguma instrução sobre como visualizar os objetos astronômicos através do telescópio. Após a realização da observação, eles foram entrevistados. A análise dos dados permitiu a elaboração de 12 categorias que foram posteriormente interpretadas com base nas relações com o saber (relação com o mundo, consigo mesmo e com o outro), conforme apresentadas por Bernard Charlot.

  11. Péndulos astronómicos y cronómetros marinos de la armada: el observatorio de San Fernando y los antecedentes del patrón nacional de tiempo (1753-1957

    Directory of Open Access Journals (Sweden)

    González González, Francisco José

    1998-06-01

    Full Text Available This article is a brief review on the precision clocks in use by the Spanish Navy during the XVIII, XIX and XX centuries. It deals with the introduction in Spain of marine chronometers needed for the application of the new techniques of astronomical navigation and also, with the evolution of the methods for time keeping and determination by astronomical pendulum clocks. Both facts placed the Navy and its Observatory in a good starting position for future activity in the field of the scientific study of time in our country.

    Este artículo presenta un breve estudio sobre los relojes de precisión usados por la Armada española durante los siglos XVIII, XIX y XX. Se trata, por una parte, sobre la introducción en España de los cronómetros marinos, necesarios para la aplicación de las nuevas técnicas de navegación astronómica. Se estudia, además, la evolución del sistema de determinación y conservación de la hora mediante péndulos astronómicos, origen del servicio horario del Observatorio de San Femando. Ambas vertientes sitúan a la Marina, y a su Observatorio, en un lugar preferente en los trabajos relacionados con el cómputo científico del tiempo en nuestro país.

  12. Astronomical Perception of the Secondary School's Students in São Paulo's State School in Suzano City. (Spanish Title: Percepción Astronómica de Alumnos de la Enseñanza Media de la Red Estatal de San Pablo en la Ciudad de Suzano.) Percepção Astronômica de um Grupo de Alunos do Ensino Médio da Rede Estadual de São Paulo da Cidade de Suzano

    Science.gov (United States)

    França de Oliveira, Edilene; Voelzke, Marcos Rincon; Amaral, Luis Henrique

    2007-12-01

    Although Astronomy is one of the oldest Sciences in the world and many of its concepts are popular, it is possible to observe that a major part of the students do not know about them. This work aims to analyse the basic knowledge of the secondary school's students of a state school in the city of Suzano, related to the astronomical phenomena, which surround them. It was carried out a questionnaire of multiple choice to 34 students from the first grade, night classes, of the state school Batista Renzi. From the sample, 34 students, only 29.4% of them could understand the succession of the days; 20.6% could explain the seasons of the year and 20.6% had some idea about celestial objects nearer to the Earth. In turn, 67.6% correctly classified the Sun as a star; 55.9% related the Big Bang to the origin of Universe; only 20.6% identified the light-year as an unit of distance and 32.4% recognized a falling star as a meteor. The actual analysis was expanded to more 310 students of other classes, grades and periods of the same school. In this first stage, it can be noted the students' little discernment of the astronomical events and mainly the great confusion about the appropriate meaning of popular astronomical terms. Aunque la Astronomía es una de las ciencias más antiguas de la humanidad y muchos de los conceptos astronómicos son populares, se observa que una parcela significativa de los estudiantes se encuentra al margen de estas informaciones. El presente trabajo pretende analizar el nivel de conocimiento básico de los alumnos de la Enseñanza Media de la Red Estatal de la ciudad de Suzano con relación a los fenómenos astronómicos que los rodean. Con este objetivo fue elaborado un formulario constando de preguntas de selección múltipla, aplicado en el primer año nocturno de la Escuela Estatal Batista Renzi. En un universo de 34 alumnos se constató que solamente 29,4% comprendían la sucesión de los días; 20,6% explicaron correctamente las estaciones del

  13. Influencia de la marea astronómica sobre las variaciones del nivel del Río Negro en la zona de Carmen de Patagones

    Directory of Open Access Journals (Sweden)

    Enrique D'Onofrio

    2010-12-01

    Full Text Available El Río Negro, límite natural entre las provincias de Buenos Aires y Río Negro, es uno de los ríos más importantes de la Patagonia que desemboca en el Océano Atlántico. Es navegable desde su desembocadura hasta Carmen de Patagones por embarcaciones de hasta 2,04 m de calado, dificultándose por irregularidades en la profundidad aguas arriba. La onda de marea proveniente del océano Atlántico ingresa al río haciendo que este adopte un régimen semidiurno hasta Carmen de Patagones. El conocimiento de la onda de marea en este tramo del río es de fundamental importancia para la calibración de modelos numéricos, el perfeccionamiento de los sistemas de alerta de inundaciones y la toma de decisiones relacionadas con el manejo costero. En este trabajo se analizan cuatro series de mediciones de marea, dos obtenidas en el hidrómetro de Carmen de Patagones con una duración de 608 y 731 días, una de 77 días proveniente de un mareómetro instalado en el kilómetro 18 del río y una de 79 días obtenida con un sensor de presión fondeado en proximidades de Punta Redonda (desembocadura del Río Negro. Se calculan y comparan los espectros de potencia de las alturas observadas en los tres sitios para detectar los cambios energéticos producidos en la banda de frecuencias correspondientes a la marea astronómica. De su comparación surge que la energía de las componentes semidiurnas y diurnas disminuye un 22% y un 45% respectivamente desde la desembocadura del Río Negro hasta Carmen de Patagones. En contraposición se observa un ligero aumento de la energía correspondiente a las frecuencias de las componentes cuarto diurnas. Esto se debe fundamentalmente a procesos no lineales inducidos por aguas someras y a irregularidades en la morfología del fondo del río. Para obtener las amplitudes y épocas de la marea se realizan análisis armónicos por el método de cuadrados mínimos. Las amplitudes de las componentes diurnas en Carmen de Patagones

  14. Arqueología del cielo. Orientaciones astronómicas en edificios protohistóricos del sur de la Península Ibérica

    Directory of Open Access Journals (Sweden)

    Esteban, César

    2013-06-01

    Full Text Available We present an archaeoastronomical analysis of the orientations of six protohistoric sanctuaries and public buildings located in archaeological sites of the south of the Iberian Peninsula (Coria del Río, El Carambolo, Saltillo, Mesa de Setefilla, Tejada la Vieja and El Oral. This study, the first of its kind conducted on a sample of Early Iron Age sanctuaries in this geographic area, is based on the accurate measurement of the orientations defined by the buildings and the analysis of the horizon around them and reveals clear astronomical relations. In particular, religious buildings show similar characteristics and orientation towards an azimuth of 55°. The regularities found seem to suggest the existence of religious beliefs and rituals linked to singular positions of the brightest celestial bodies as the Sun, Moon or Venus.Presentamos un análisis arqueoastronómico de la orientación de seis santuarios y edificios de carácter público protohistóricos en sitios arqueológicos situados en el mediodía de la Península Ibérica (Coria del Río, El Carambolo, Saltillo, Mesa de Setefilla, Tejada la Vieja y El Oral. El estudio, el primero de este tipo que se realiza sobre una muestra de santuarios del Hierro Antiguo en esta área geográfica, se basa en la medida precisa de las orientaciones definidas por los edificios y el análisis del horizonte que les rodea y revela claros vínculos astronómicos. En particular, los edificios de culto muestran unas características similares y una orientación hacia un acimut de 55°. Las regularidades encontradas parecen sugerir la posible existencia de credos y rituales religiosos relacionados con posiciones singulares de los astros principales visibles a simple vista, como el Sol, la Luna o Venus.

  15. Nicolás Mascardi e a carta-relación de 1670: uma análise preliminar das observações astronômicas realizadas pelo missionário jesuíta = Nicolás Mascardi and the carta-relación de 1670: a preliminary analysis of astronomical observations carried out by the jesuit missionary

    Directory of Open Access Journals (Sweden)

    Biehl, Maico

    2014-01-01

    Full Text Available O presente artigo apresenta os resultados preliminares da pesquisa que venho desenvolvendo como bolsista PIBIC/CNPq junto ao projeto “Uma ordem de homens de religião e de ciência: difusão, produção e circulação de saberes e práticas científicas pela Companhia de Jesus (América meridional, séculos XVII e XVIII”. O subprojeto prevê o contato com as teorias astronômicas vigentes no Seiscentos e no Setecentos, com as obras de Astronomia que integravam os acervos da Ordem e com os estudos produzidos por missionários já no Novo Mundo. Assim como, a reconstituição das trajetórias de jesuítas que realizaram observações astronômicas nas reduções em que atuaram, compartilhando os seus estudos através da prática epistolar ou por meio de obras. Neste artigo, especificamente, me detenho em reconstituir brevemente a trajetória do jesuíta Nicolas Mascardi, destacando as observações astronômicas que realizou na América e as suas comunicações com demais estudiosos da astronomia.

  16. Sobre os céus e as marés do Pacífico: as observações astronômicas do jesuíta Nicolás Mascardi (Chile, século XVII

    Directory of Open Access Journals (Sweden)

    Eliane Cristina Deckmann Fleck

    2014-12-01

    Full Text Available A atuação da Companhia de Jesus na América espanhola e portuguesa constitui-se em tema de várias investigações e obras, nas quais merece destaque a dedicação de seus religiosos ao ensino e à catequese. Alguns membros da Ordem, no entanto, se dedicaram, também, a observações de fenômenos naturais, da fauna e da flora nativas e, ainda, a aspectos da geografia dos territórios em que atuaram, legando-nos uma série de estudos informados através de cartas, relatórios ou obras. Nosso propósito neste artigo é o de apresentar e analisar os registros que o padre jesuíta italiano Nicolás Mascardi fez de suas observações astronômicas e, em especial, do estudo que realizou sobre as marés do arquipélago de Chiloé durante os anos em que atuou na então Vice-Província Jesuítica do Chile, no século XVII.

  17. Evaluation of Cardiovascular Risk Scores Applied to NASA's Astronant Corps

    Science.gov (United States)

    Jain, I.; Charvat, J. M.; VanBaalen, M.; Lee, L.; Wear, M. L.

    2014-01-01

    In an effort to improve cardiovascular disease (CVD) risk prediction, this analysis evaluates and compares the applicability of multiple CVD risk scores to the NASA Astronaut Corps which is extremely healthy at selection.

  18. Tratamiento formal de imágenes astronómicas con PSF espacialmente variable

    Science.gov (United States)

    Sánchez, B. O.; Domínguez, M. J.; Lares, M.

    2017-10-01

    We present a python implementation of a method for PSF determination in the context of optimal subtraction of astronomical images. We introduce an expansion of the spatially variant point spread function (PSF) in terms of the Karhunen Loève basis. The advantage of this approach is that the basis is able to naturally adapt to the data, instead of imposing a fixed ad-hoc analytic form. Simulated image reconstruction was analyzed, by using the measured PSF, with good agreement in terms of sky background level between the reconstructed and original images. The technique is simple enough to be implemented on more sophisticated image subtraction methods, since it improves its results without extra computational cost in a spatially variant PSF environment.

  19. IAA : Información y actualidad astronómica (10)

    OpenAIRE

    Agudo, Iván; López de Lacalle, Silbia; Jaramillo, José Luis; López-Valverde, M. A.; Alfaro, Emilio J.; Vílchez Medina, José Manuel; López-Moreno, José Juan; Agudo, Iván

    2003-01-01

    Sumario : Investigación: Chorros relativistas en núcleos activos de galaxias.-- Materia oscura: a tientas por el Universo.-- Ventana Abierta: Físico teórico autónomo se ofrece para.-- Charlas con… Robert Haberle.-- Actualidad Científica: La búsqueda de las estrellas más viejas de la Galaxia.-- Un superbólido más brillante que la Luna llena surcó el cielo argelino.-- Actividades IAA.-- Agenda.

  20. Effects of Long Duration Spaceflight on Venous and Arterial Compliance in Astronants

    Science.gov (United States)

    Platts, Steven; Ribeiro, L. Christine

    2014-01-01

    1. Project Overview Visual impairment and intracranial pressure (VIIP) is a spaceflight-associated medical condition affecting at least a third of American astronauts who have flown International Space Station (ISS) missions. VIIP is defined primarily by visual acuity deficits and anatomical changes to eye structures. In some astronauts, eye-related changes do not revert back to the preflight state upon return to Earth. Our team will study some of the possible causes for this syndrome. This will be achieved by reviewing previous astronaut data for factors that may predispose astronauts to higher rates of developing this syndrome or greater severity of symptoms. Additionally, we will conduct 3 separate experiments that will characterize vessels in the head and neck and measure the effects of the experimental conditions on ocular structures and function. 2. Technical Summary The primary objective of this study is to determine whether vascular compliance is altered by spaceflight and whether such adaptations are related to the incidence of the VIIP. In particular, we will measure ocular parameters and vascular compliance in vessels of the head and neck in astronauts who have no spaceflight experience (Ground), in astronauts before, during, and after spaceflight (Flight), and in bed rest subjects with conditions similar to spaceflight (Bed Rest). Additionally, we will analyze astronaut data from the Lifetime Surveillance of Astronaut Health (LSAH) archives to determine which factors might be predictive of the development of VIIP (Data Mining). The project will be conducted in four separate, but related parts. Hypothesis The central hypothesis of this proposal is that exposure to the spaceflight environment aboard the ISS may lead to development of the VIIP syndrome (increased intracranial pressure and impaired visual acuity) and that this may be related to alterations in venous and/or arterial compliance in the head and neck. Specific Aims 1. To determine whether noninvasive measures of venous and arterial compliance are altered by long-duration spaceflight exposure in ISS astronauts and whether these changes are related to the development of the VIIP syndrome. (Flight) 2. To determine whether previous spaceflight experience predispose astronauts to lower venous compliance and/or the development of the VIIP syndrome. (Ground + Flight) 3. To use a 14-day, 6deg head-down-tilt bed rest as a model of spaceflight, to evaluate the effect of aging on vascular compliance using a subject population similar to younger (25-35 yr) and older (45-55 yr) astronaut cohorts. (Bed Rest) 4. To determine what factors contribute to lower venous compliance and/or the development of the VIIP syndrome in astronauts. (Data Mining) 3. Earth Applications This research may inform the mechanisms that regulate blood/fluid flow in and out of the brain in the head and neck. This information may help with understanding of the mechanisms behind idiopathic intracranial hypertension. 4. Link to NASA Taskbook Entry Not Yet Available

  1. Influencias socioculturales en conceptos astronómicos: el caso del horizonte en la reforma copernicana

    Science.gov (United States)

    Szapiro, A.

    2017-10-01

    I analyze the meaning given by Ptolemy to the concept of horizon; especially how it allowed him to prove, through astronomical observations, the central position of the Earth in the Universe. I review the ways in which Copernicus and Galileo gave heliocentric answers to the Ptolemaic proof. I show that Galilean solution entailed a radical conceptual change, which brought with it a new sense to the concept of horizon. I state that this change was the product of sociocultural influences of the period.

  2. IAA : Información y actualidad astronómica (35)

    OpenAIRE

    Guerrero, Martín A.; Gutiérrez, Pedro J.; Villar-Martin, Montse; Gutiérrez Vela, Yael; Laguillo Diego, Alejandra; Aguayo Díaz, Alberto; Prior, Marcos; Márquez, Isabel; García, Emilio José; Ascaso, Begoña; López de Lacalle, Silbia; Estupinyà, Pere; Abril, Miguel; Barceló, Carlos

    2011-01-01

    Sumario : Nebulosas planetarias.-- ¿Solo 25 años de ciencia cometaria?.-- Leyendo entre líneas (I).-- DECONSTRUCCIÓN Y otros ENSAYOS. La física del Correcaminos.-- EL “MOBY DICK” DE... Isabel Márquez (IAA-CSIC).-- CIENCIA EN HISTORIAS. La ciencia es un fraude...desde siempre.-- ACTUALIDAD.-- ENTRE BASTIDORES.-- SALA LIMPIA.-- CIENCIA: PILARES E INCERTIDUMBRES. Agujeros negros.-- AGENDA/RECOMENDADOS.

  3. IAA : Información y actualidad astronómica (50)

    OpenAIRE

    López de Lacalle, Silbia; Villar-Martin, Montse; Delgado, Miguel Ángel; Duffard, René D.; Claret dos Santos, Antonio; Pérez-Torres, Miguel A.; Moreno, Fernando; Sánchez, Alejandro; Abril, Miguel

    2016-01-01

    Sumario : El exoplaneta más cercano.-- La Tierra desde el cielo.-- Plutón: quién te ha visto y quién te ve.-- DECONSTRUCCIÓN Y otros ENSAYOS. El tiempo de vida de las estrellas masivas.-- CIENCIA EN HISTORIAS...Vera Rubin, curvas de rotación galáctica y materia oscura.-- EL “MOBY DICK” DE... Fernando Moreno (IAA).-- ACTUALIDAD.-- CIENCIA: PILARES E INCERTIDUMBRES. Contaminación lumínica...21 SALA LIMPIA.

  4. IAA : Información y actualidad astronómica (27)

    OpenAIRE

    Schödel, Rainer; López de Lacalle, Silbia; Villamariz Cid, Charo; Pérez-Torres, Miguel A.; Alberdi, Antxón; Amado, Pedro J.; Muñoz, Olga; López-Valverde, M. A.; Duffard, René D.; López Guerrero, José Antonio; Barceló, Carlos; Maíz Apellániz, Jesús

    2009-01-01

    Sumario : Sagitario A*: el agujero negro en el corazón de la Vía Láctea.-- ESPECIAL: Año Internacional de la Astronomía.-- HISTORIAS DE ASTRONOMÍA. Chandrasekhar y los agujeros negros.-- DECONSTRUCCIÓN Y otros ENSAYOS. Binarias de rayos X.-- EL “MOBY DICK” DE...Pedro Amado.-- ACTUALIDAD.-- ENTRE BASTIDORES.-- CIENCIA: PILARES E INCERTIDUMBRES. El tiempo.-- ACTIVIDADES IAA.

  5. About the Sociedade Astronômica Brasileira and its 36th annual meeting (2011)

    Science.gov (United States)

    Janot-Pacheco, E.

    2012-12-01

    We present an overview of the Brazilian Astronomical community and of its available observational facilities. We explain how is organized the Brazilian Astronomical Society (S.A.B.) and present some information on our last annual meeting, held in 2011.

  6. Reporte de actividades de la Estación Astronómica Polar ``J.L.Sersic''

    Science.gov (United States)

    Mosconi, M.; Recabarren, P.; Ferreiro, D.; Renzi, V.; Ozu, R.

    The ``J.L.Sersic" Astronomy Polar Station, dedicated to measure environmental parameters, which describes the sky quality for astronomical purposes, operates at 78 degrees South, in Belgrano Station, since the '94/'95 Antarctic Summer Campaign. The activities are developed during the darkness period between April and August. We measure meteorological parameters, seeing, extinction coefficients and we make a monitoring of Eta Carinae. This site registers the lowest temperatures among the argentine permanent stations, and has the most stable weather conditions with continuously dark periods of several dozens of hours. The average seeing is of the order of 3.8 arc seconds, with some occasional measurements less than an arc second. The best conditions are observed at the beginning and at the end of the winter period, being the best behavior in the V and I bands. The differences on the luminosity of the stars at different HA is not too notable at high latitudes. Due to the small difference of the air mass for different HA at high latitudes, there is a very small variation in the star luminosity. So, we have not used the traditional method. We decided to apply the method of Harris et al. (1981), which is based on the treatment by mean squares of a matrix obtained from the observations of groups of objects at different heights. We obtain K coefficients, which are function of the first order coefficients (k'), of the second order (k'') and the color index (IC): K=k'+k".IC. The annual average values for '97 and '98, in the U,V,B,R,I bands, are: Year/Coeff. & K & Kv & Kb & Ku & Kr 1997 & 0.4629 & 0.3245 & 0.3668 & 0.689 & 0.5647 1998 & 0.4313 & 0.4335 & 0.4143 & 0.876 & 0.3698 The analysis of the obtained results shows that the atmosphere is unstable and too turbulent for many astronomical works. The seeing is not good enough and the extinction in the different bands is high. Belgrano Station is located inside the auroral oval and below of the ``ozone hole". Both phenomenon affect the observed parameters. The behavior of the U band and its relationship with the variations of the ozono layer and the auroral activity are very interesting subjects to be studied.

  7. Del Observatorio Astronómico a la Virgen de Atocha (Madrid): una historia de oportunidades perdidas

    OpenAIRE

    Herranz Duránez, Luisa

    2017-01-01

    La Glorieta del Emperador Carlos V, coloquialmente conocida con su anterior nombre como Glorieta de Atocha, es uno de los espacios urbanos más importantes de la capital. Lo que en origen suponía el límite de la ciudad, materializado tanto en una cerca administrativa como en una topografía escarpada que se precipitaba hacia la llanura manchega; es hoy puerta céntrica de visitantes y turistas, nudo de comunicaciones, paseo del arte, albergue tanto de edificios institucionales y representativos ...

  8. Conservación de material histórico sobre papel en el Observatorio Astronómico de la Universidad Nacional de Córdoba

    Science.gov (United States)

    Laguzzi, N.; Tonini, A.; Andreoli, G.; Goldes, G.; Paolantonio, S.; Cequeira, F.; Landi, L.; Alba, J.

    At the recently created Astronomical Museum ``Pte. Sarmiento - Dr. Benjamin Gould", the task of preventive conservation of historic documents has been faced. These materials include: 1) letters exchanged between national authorities and the directors of the Observatory, during the first decades (1870-1880-1890); b) original observation logs from these very first times, containing astrometrical and photometrical data; c) a variety of ancient books and papers; d) administrative documents. The state of conservation of this patrimony was varied: since well-conserved books and letters, to highly degraded logs. The observation logs written by B. Gould and the astronomers who followed him had been stocked in a safe with a permanent humidity of about 70 %, without any ventilation and exposed to the attack of insects of the family ``dermestidae." These conditions could not be worse for the conservation of paper. In order to stop the proccess of degradation and create a healthy environment for written-paper conservation, a team was formed with personnel belonging to the Cultural Area of the Municipality. The tasks being performed on the observation logs are: 1) an initial, mechanical cleaning, performed once the material is extracted from the contaminated safe: by these means, adult insects and pupas are removed 2) a stage of about two weeks of duration, in which the logs are mantained in a vacuum chamber, in orden to completely eliminate the adult, pupa and egg stage insects by anoxia 3) the final mechanical cleaning 4) storage in a clean location. In order to perform these tasks, we work in collaboration with the Environmental Observatory of the City, and the group of Material-Science Research of Fa.M.A.F. Regarding the letters, a mechanical cleaning was performed. After that, the letters were digitized by means of a scanner, inventoried, put inside acid-free polipropylene envelops and filed for conservation, protected from intense light and external sources of contamination. Copies of these letters will be included as exhibits.

  9. Extracción de conocimiento en bases de datos astronómicas mediante redes de neuronas artificiales: aplicaciones en la misión Gaia

    Science.gov (United States)

    Fustes Villadóniga, Diego

    2014-02-01

    In the so-called IT era, the capabilities of data acquisition systems have increased to such an extent that it has become difficult to store all the information they produce, and analyse it. This explosion of data has recently appeared in the field of Astronomy, where an increasing number of objects are being observed on a regular basis. An example of this is the upcoming Gaia mission, which will pick up multiple properties of a billion stars, whose information will have a volume of approximately a petabyte. The analysis of a similar amount of information inevitably requires the development of new data analysis methods to extract all the knowledge it contains. This thesis is devoted to the development of data analysis methods to be integrated in the Gaia pipeline, such that knowledge can be extracted from the data collected by the mission. In order to analyze the data from the Gaia mission, the European Space Agency organized the Data Processing and Analysis Consortium (DPAC) which is composed of hundreds of scientists and engineers. DPAC is divided into eight Coordination Units (CUs). This thesis is dedicated to algorithm development in CU8, which is responsible for source classification and astrophysical parameters (AP) estimation. Methods based on Artificial Neural Networks (ANNs) are developed to perform the tasks related to two different work packages in CU8: the GSP-Spec package (GWP-823), and the OA package (GWP-836). The GSP-Spec package is responsible for estimating stellar APs by means of the Radial Velocity Spectrograph (RVS) spectrum. This work presents the development of one of the GSP-Spec modules, which is based on the application of feed-forward ANNs. A methodology is described, based on the optimization of genetic algorithms and aimed at obtaining an optimal set of configuration parameters for the ANN in each case, depending on the signal to noise ratio (SNR) in the RVS spectrum and on the type of star to parameterize. Furthermore, in order to improve the AP estimates, wavelet signal processing techniques, applied to the RVS spectrum, are studied. Despite the effectiveness shown by ANNs in estimating APs, in principle they lack the ability to provide an uncertainty value on these estimates, making it impossible to determine their reliability. Because of this, a new architecture for the ANN is presented in which the inputs and outputs are reversed, so that the ANN estimates the RVS spectrum from the APs. Such an architecture is called Generative ANN (GANN) and is applied to the AP estimation of a set of simulated RVS spectra for the Gaia mission, where it is more effective than the conventional ANN model, in the case of faint stars with low SNR. Finally, the GANN can be applied for obtaining the posterior probability of each of the APs according to the RVS spectrum, allowing for their more complete analysis. Given the nature of the Gaia mission, which is the first astronomical mission that will observe, in an unbiased way, the entire sky up to magnitude 20, a large number of outliers are expected. The OA package in CU8 handles the processing of this type of objects, which are defined as those that could not be reliably classified by the methods in the upstream classification packages. OA methods are based on the unsupervised learning of all outliers. Such learning has two parts: clustering and dimensionality reduction. The Self-Organizing Map (SOM) algorithm is selected as a basis for this learning. Its effectiveness is demonstrated when it is applied, with an optimal configuration, to the Gaia simulations. Furthermore, the algorithm is applied to real outliers from the SDSS catalog. Since a subsequent identification of the clusters obtained by the SOM is necessary, two different methods of identification are applied. The first method is based on the similarity between the SOM prototypes and the Gaia simulations, and the second method is based on the recovery of stored classifications in the SIMBAD catalog by cross-matching celestial coordinates. Thanks to the visualization of the SOM planes, and to both

  10. La enseñanza-aprendizaje de fenómenos astronómicos cotidianos en la Educación Primaria española

    Directory of Open Access Journals (Sweden)

    J. M. Vílchez-González

    2015-01-01

    Full Text Available En este articulo se presentan los resultados de un estudio realizado con un grupo clase integrado por alumnos espanoles de educacion primaria (7-8 anos de una escuela concertada de Granada capital, en relacion con el sistema Sol-Tierra-Luna. Se analiza el cambio conceptual en la interpretacion de fenomenos cotidianos (ciclo dianoche, fases lunares y estaciones en tres grupos de segundo curso con metodologias de aprendizaje diferenciadas. Se lleva a cabo un estudio longitudinal, durante mas de dos trimestres, mediante la realizacion de un pretest y dos postests. Segun muestran nuestros resultados, hay considerables obstaculos cognitivos para la comprension de estos fenomenos. Al parecer, las estrategias didacticas interactivas basadas en juego de rol son las que ofrecen mejores resultados a corto y a largo plazo.

  11. Mesa redonda: Argentina en proyectos globales de investigaciones espaciales y astronómicas. Astronomía óptica en Argentina

    Science.gov (United States)

    Folatelli, G.

    2016-08-01

    This is a brief summary of the current status of observational astronomy in the optical range in Argentina, as seen by the author. This roundtable presentation aimed at setting off the discussion within the community about the issue of observational facilities and its posible solutions.

  12. Mesa redonda: Argentina en proyectos globales de investigaciones espaciales y astronómicas. Uso científico de la Antena de Espacio Profundo DSA 3

    Science.gov (United States)

    Colazo, M.

    2016-08-01

    Argentine has 10 percent of the operative time available for the DSA 3 Antenna of the European Space Agency, installed in Malargüe, Mendoza. Here we present the history of the project and the current activities for the scientific use of the antenna.

  13. Active Galactic Nuclei Feedback and Clusters Biman B. Nath

    Indian Academy of Sciences (India)

    Not. R. Astron. Soc., 365, 509. Mazzotta, P., Rasia, E., Moscardini, L., Tormen, G. 2004, Mon. Not. R. Astron. Soc., 354, 10. Nath, B. B., Roychowdhury, S. 2002, Mon. Not. R. Astron. Soc., 333, 145. Nath, B. B., Majumdar, S. 2011, Mon. Not. R. Astron. Soc., 416, 279. Navarro, J. F., Frenk, C. S., White, S. D. M. 1997, Astrophys.

  14. Conocimientos astronómicos del profesorado de educación secundaria obligatoria y preferencias metodológicas para la enseñanza de astronomía

    Directory of Open Access Journals (Sweden)

    José Luis GARCÍA HERRERO

    2014-11-01

    Full Text Available La astronomía forma parte del currículo de las materias científicas en la educación obligatoria, incluyendo básicamente unos pocos conceptos tradicionales como las estaciones del año, las fases lunares, los movimientos de la Tierra, los eclipses…, y dejando de lado otros más actuales como los exoplanetas y la cosmología. Este artículo pretende estudiar en primer lugar el nivel de conocimientos básicos sobre astronomía del profesorado de Educación Secundaria Obligatoria (ESO, con el fin de detectar posibles carencias formativas y concepciones alternativas. En el estudio participaron profesores de especialidades científicas y no científicas de dicha etapa. Posteriormente se realizó un análisis de correlación de resultados en función de diversas variables, y además se comparó con los resultados obtenidos por un extenso grupo de alumnos de ESO. En segundo lugar, el artículo se centra en estudiar las preferencias metodológicas para la enseñanza-aprendizaje de astronomía, contando con los mismos participantes que en el caso anterior, y con el objetivo de conocer sus valoraciones sobre diferentes propuestas, en algunos casos bastante innovadoras. Los resultados obtenidos pueden ser orientativos para estudios posteriores de mayor envergadura, de cara a la determinación de necesidades de formación específicas en astronomía en el caso de docentes de materias científicas. Además, serán de utilidad como orientaciones metodológicas a la hora de abordar la enseñanza de la astronomía.

  15. Maximum mass ratio of am CVn-type binary systems and maximum white dwarf mass in ultra-compact x-ray binaries (addendum - Serb. Astron. J. No. 183 (2011, 63

    Directory of Open Access Journals (Sweden)

    Arbutina B.

    2012-01-01

    Full Text Available We recalculated the maximum white dwarf mass in ultra-compact X-ray binaries obtained in an earlier paper (Arbutina 2011, by taking the effects of super-Eddington accretion rate on the stability of mass transfer into account. It is found that, although the value formally remains the same (under the assumed approximations, for white dwarf masses M2 >~0.1MCh mass ratios are extremely low, implying that the result for Mmax is likely to have little if any practical relevance.

  16. Comparación del funcionamiento entre PMT y SiPM para la detección de Cherenkov atmosférico en el Complejo Astronómico El Leoncito

    Science.gov (United States)

    Yelós, L. D.; Suarez, F.; García, B.

    2017-10-01

    Most recent discoveries in gamma ray astronomy with energies around 50 GeV to 30 TeV, were achieved with ground Cherenkov Telescopes, traditionally composed of a parabolic mirror and a single or an array of photo multiplier tubes (PMTs) in their focus. The same detectors (or similar) are used in most astrophysics experiments. Recently, a new detector, the silicon photo-multiplier (SiPM), is progressively replacing the PMTs due to their technical advantages. However some limitations in their functioning make them more complex to use than PMTs and forces their characterization for each project. This work describes the characterization of SiPM from SensL (model MicroFC-SMA-30035) and a PMT from Hamamatsu (model R1463), both detectors are possible options to be used in an array of three Cherenkov telescopes at CASLEO. Additionally, we include the results of the operation of both detectors under controlled laboratory conditions that simulate expected conditions at field. Laboratory test were run in a darkbox with a data acquisition system, a personalized data analyze system with ROOT libraries, temperature control and monitoring, polarization control, a controlled light source, and humidity monitoring.

  17. Desarrollo de una Interfaz de Control para un Observatorio Astronómico Robotizado con fines educativos en la Facultad de Ciencias Exactas; Físicas y Naturales de la UNSJ

    Science.gov (United States)

    Pogrebinsky, L.; Francile, C.

    We report the development and the construction of an Interface to Control a robotized Astronomical Observatory (ICOA), which allows to control the operation of an observatory based on a Meade LX200 telescope. The interface operates together with a computer to control and supervise all the local variables of the observatory, and can take the control of it in risky situations. It serves as a link among the control computer and all the necessary devices for the astronomical observation such as the telescope, the dome, the weather station, the CCD camera, the calibration devices and the security devices. The computer receives orders from an operator who can be or not at the site of observation. The goal of this robotized observatory is the operation in a secure, autonomous and unattended way, with the purpose of to be used remotely by the students of the "Facultad de Ciencias Exactas, Físicas y Naturales" of the UNSJ. FULL TEXT IN SPANISH

  18. Análisis, estudio y conservación de los edificios astronómicos mayas. Arquitectura maya y urbanismo, una aproximación desde la astronomía y el paisaje.

    OpenAIRE

    MAY CASTILLO, MANUEL

    2016-01-01

    El presente trabajo representa el resultado final de seis años de investigación en la región maya y versa sobre las relaciones entre la arquitectura y el urbanismo con el paisaje y la astronomía. En una primera parte se presentan los fundamentos metódicos para el estudio de la arquitectura y el urbanismo maya, a partir de la lectura de los datos del paisaje circundante y las orientaciones arquitectónicas. A lo anterior se le suman los datos provistos por las fuentes pr...

  19. Fluctuaciones interanuales a multidecádicas de la temperatura de verano en el centro-oeste de Argentina y procesos atmosféricos/oceánicos/astronómicos globales

    Directory of Open Access Journals (Sweden)

    Eduardo Andres Agosta

    2008-12-01

    Full Text Available La temperatura estival (octubre-marzo en la región Centro-Oeste de Argentina (COA, 28°-36°S y 65°-70°O tiene un comportamiento espacial coherente y temporal en fase, en escalas interanuales a interdecádicas (Agosta y otros 2004. Se encuentra que la temperatura del aire presenta cuasi-oscilaciones significativas en las bandas de 11 años y 18 años aproximadamente. La primera se vincula al forzante solar, la segunda, a los efectos de la transición climática de 1976/77 (IPCC, 2001. Esta transición afectó transitoriamente la variabilidad de baja frecuencia de la temperatura como fenómeno de interferencia sobre el cuasi-ciclo solar de 11 años dominante.The summer (Oct-Mar temperature in Central-West Argentina (CWA, 28°-36°S y 65°-70°W shows a behaviour spatially coherent and temporally in phase at interannual to interdecadal scales. (Agosta et al. 2004. It is found the air temperature shows significant cuasi-oscillations in the spectral bands of roughly 11-yr. and 18- yr. The former is linked to the solar forcing, the latter to the effects of the climate transition of the summer 1976/77 (IPCC 2001. This transition transitorily affected the low-frequency variability of the temperature as an interference phenomenon upon the cuasi-11-yr.-solar cycle domain.

  20. An Interferometric Study of the Post-AGB Binary 89 Herculis. 1: Spatially Resolving the Continuum Circumstellar Environment at Optical and Near-IR Wavelengths with the VLTI, NPOI, IOTA, PTI, and the CHARA Array

    Science.gov (United States)

    2013-01-01

    Frankowski, A., & Jorissen, A. 2007, Balt . Astron., 16, 104 Fukagawa, M., Hayashi, M., Tamura, M., et al. 2004, ApJ, 605, L53 Fukagawa, M., Tamura, M...Kenyon, S. J., & Hartmann, L. 1987, ApJ, 323, 714 Kipper, T. 2011, Balt . Astron., 20, 65 Königl, A. 1999, New Astron. Rev., 43, 67 Kraus, S

  1. f(cm) =

    Indian Academy of Sciences (India)

    [5] S Chandra, W H Kegel, R J Le Roy and T Hertenstein, Astron. Astrophys. Suppl. 114, 175 (1995). [6] S Chandra, U V Maheshwari and A K Sharma, Indian J. Pure Appl. Phys. 34, 925 (1996). [7] S Chandra, U V Maheshwari and A K Sharma, Astron. Astrophys. Suppl. 117, 557 (1996). Pramana – J. Phys., Vol. 56, No.

  2. Phase-Resolved Spectra of PSR B0525+21 and PSR B2020+28 JL ...

    Indian Academy of Sciences (India)

    Jiao-Ke (2009)), GDUPS (2009) and NFSC project 10673021. References. Chen, J. L. et al. 2007, Chinese J. Astron. Astrophys., 7, 789. Cordes, J. M. 1978, Astrophys. J., 222, 1006. Kuzmin, A. D., Izvekova, V. A., et al. 1998, Astron. Astropys.

  3. The galactic luminous supersoft X-ray source RXJ0925.7-4758 / MR ...

    Indian Academy of Sciences (India)

    Nandita Prodhani

    2018-01-30

    Jan 30, 2018 ... ... F Verbunt and C Motch, Astron. Astrophys. 385, 511 (2002). [27] C Motch, H Bearda and C Neiner, Astron. Astrophys. 393, 913 (2002). [28] G J Ferland, R L Porter, P A M van Hoof, R J R Williams,. N P Abel, M L Lykins, G Shaw, W J Henney and P C. Stancil, Revista Mexicana de Astronomia Y Astrofisia.

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

    Indian Academy of Sciences (India)

    P. Kishore

    2017-06-19

    Jun 19, 2017 ... Suzuki, S., Dulk, G. A. 1985, in: Solar Radiophysics, edited by D. J. McLean & N. R. Labrum, Cambridge University. Press, Cambridge, p. 289. Trottet, G., Pick, M., House, L., Illing, R., Sawyer, C., Wag- ner, W. 1982, Astron. Astrophys., 111, 306. Vršnak, B., Magdalenic, J., Zlobec, P. 2004, Astron. Astro- phys.

  5. Hingega klaverite duell Tartus / Alo Põldmäe

    Index Scriptorium Estoniae

    Põldmäe, Alo, 1945-

    2011-01-01

    Klaverimuuseumi ja Tartu Saksa Kultuuri Instituudi koostöös 3. detsembril toimunud muusikaõhtust "Hingega klaverid - ajaloorännakud eesti ja saksa klaveritel", kus fookuses olid tiibklaverid Astron (eesti) ja Bechstein (saksa)

  6. Star Formation in Galaxies: Proceedings of a Conference Held in Pasadena, California

    Science.gov (United States)

    1987-05-01

    see Nussbaumer et al. 1982). Their spectra are not available in the IUE spectral atlas and are not included in our models. 2.2 Comparison with...1983) Astron. Astrophys., 120, 113. Nussbaumer , H., Schmutz, W., Smith, L.J., and Willis, A.J. (1982), Astron. Astrophys. Suppl., 117, 257. Rosa, M...Jim Cordes, Martin Harwit, and Martha Haynes at Cornell for useful discussions; Barbara Boettcher for her help with the figures; and Sylvia Corbin

  7. REVISTA MEXICANA DE ASTRONOMÍA Y ASTROFÍSICA, A REAL OPTION FOR ASTRONOMICAL PUBLICATION

    OpenAIRE

    S. Torres-Peimbert; C. Allen

    2011-01-01

    Presentamos datos estadísticos sobre la Revista Mexicana de Astronomía y Astrofísica. Consideramos que esta publicación está bien posicionada en la literatura astronómica internacional. Igualmente, presentamos información sobre la Serie de Conferencias, que ha tenido muy amplia aceptación en la comunidad astronómica.

  8. Estimate of stellar masses from their QPO frequencies

    Indian Academy of Sciences (India)

    [27] T Klahn, D Blaschke et al, Phys. Rev. C74, 035802 (2006). [28] D J Nice et al, Astrophys. J. 634, 1242 (2005). [29] F Özel, Nature 441, 1115 (2006). [30] T Belloni, M Méndez and J Homan, Astron. Astrophys. 437, 209 (2005). [31] T Belloni, M Méndez and J Homan, Mon. Not. R. Astron. Soc. 376, 1133 (2007), arXiv:astro-.

  9. Space Telescopes

    Science.gov (United States)

    2010-01-01

    Proc 6317:OT1–OT9 Serlemitsos PJ, Jahota L, Soong Y (plus 14 authors) (1995) The X-ray telescope on board ASCA. Pub Astron Soc Jap 47:105–114...Serlemitsos PJ, Soong Y, Chan K-W (plus 31 authors) (2007) The X-ray telescope on board Suzaku. Pub Astron Soc Jap 59:9–21 Shimizu T (2004) Solar-B solar

  10. Galex and Optical Observations of GW Librae during the Long Decline from Superoutburst

    Science.gov (United States)

    2011-03-01

    PASJ, 60, 23 Kepler, S. O. 1993, Balt . Astron., 2, 515 Martin, D. C., et al. 2005, ApJ, 619, L1 Mukadam, A. S., et al. 2010a, ApJ, 714, 1702 Mukadam, A... Balt . Astron., 9, 231 van Zyl, L., et al. 2004, MNRAS, 350, 307 Warner, B., & van Zyl, L. 1998, in IAU Symp. 185, New Eyes to See Inside the Sun and

  11. VIMOS Integral Field Spectroscopy of Gaseous Nebulae in Local Group Dwarf Galaxies

    Science.gov (United States)

    Held, E. V.; Gullieuszik, M.; Saviane, I.; Sabbadin, F.; Momany, Y.; Rizzi, L.; Bresolin, F.

    The study of very metal-poor dwarf irregular (dIrr) galaxies is fundamental to test the cosmological scenarios of galaxy formation. Among Local Group galaxies, Leo A and SagDIG are probably the most metal-poor dwarfs, as suggested by estimates of their nebular abundances based on the empirical method [I. Saviane, L. Rizzi, E.V. Held, F. Bresolin, Y. Momany in Astron. Astrophys. 390, 59 (2002); E.D. Skillman, R. Terlevich, J. Melnick in Mon. Not. R. Astron. Soc. 240, 563 (1989); L. van Zee, E.D. Skillman, M.P. Haynes in Astrophys. J. 637, 269 (2006)].

  12. Traduzir o intraduzível: o impacto dos textos sagrados orientais no ocidente

    Directory of Open Access Journals (Sweden)

    Felipe Santos

    2009-12-01

    no século XV, ou a dos novos mundos astronômicos, físicos e da história natural ao longo da Idade Moderna. As principais consequências da vitória da Filologia se fizeram sentir no mundo da teologia e da filosofia.

  13. Extracting Information from the Gravitational Redshift of Compact ...

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Author Affiliations. Paul D. Nuñez1 Marek Nowakowski2. Department of Physics & Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112 and Observatorio Astronómico, Universidad Sergio Arboleda, Cll. 74 No. 14–14, Bogotá, Colombia. Departamento de Física, Universidad de los Andes, ...

  14. Chandrasekhar–Kendall functions in astrophysical dynamos

    Indian Academy of Sciences (India)

    him to the question [12] “Can the time of decay of 14,000 years, in the absence of internal motions, be prolonged to 500,000 years (say) by velocities of reasonable magnitude and ..... Pogorelov, E Audit and G P Zank (Astron. Soc. Pac., San Francisco, 2010) p. 28. [47] S Chandrasekhar, Phil. Trans. R. Soc. London, Ser.

  15. Sulfuric Acid on Europa's Surface and the Radiolytic Sulfur Cycle

    Science.gov (United States)

    Carlson, R.; Johnson, R.; Anderson, M.

    1999-01-01

    Galileo infrared spectra of Europa's surface show distorted water bands that have been attributed to hydrated evaporite salts (McCord et al., J. Geophys. Res. 104, 11827, 1999) or to the scattering properties of ice (Dalton and Clark, Bull. Am. Astron. Soc. 30, 1081, 1998).

  16. Know the Star, Know the Planet

    Science.gov (United States)

    2011-11-01

    detected. The astrometry and photometry of all resolved systems are listed in Table 1. For each star, we list the Washington Double Star (WDS) number...Angular Resolution Astron- omy at Georgia State University. This research made use of the Washington Double Star Catalog, maintained at the U.S. Naval

  17. The Large Scale Structure: Polarization Aspects R. F. Pizzo

    Indian Academy of Sciences (India)

    e-mail: pizzo@astron.nl. Abstract. Polarized radio emission is detected at various scales in the ... are located at the nodes of the filamentary large-scale structure of the cosmic web and form by subsequent merging .... After calibration, we produced Q and U channel images for each dataset and we inspected them to remove ...

  18. Satellite Moisture Retrieval Techniques. Volume 2. Atmospheric Sounding Bibliography

    Science.gov (United States)

    1983-01-01

    RADIATION THROUGH THE LOW ATMOSPHERE Tomasi, C; Vittori ,0. Sezione Microfisica Atmosfera , Ifa Cnr, Bologna, Italy Mem. Soc. Astron. Ital. (Italy...IMPROVED VOIGT ALGORITHM Van Derwook, Peter Clark (Masters Thesis) Texas University (May 1977) 37. A TECHNIQUE FOR ESTIMATING ATMOSPHERIC MOISTURE...AN IMPROVED VOIGT ALGORITHM Van Derwook, Peter Clark (Masters Thesis) Texas University (May 1977) 43 REMOTE SENSING ATMOSPHERIC SOUNDING OF THE

  19. Einstein -coefficients for rotational transitions in the ring-chain ...

    Indian Academy of Sciences (India)

    1994). [5] S Chandra and Rashmi, Astron. Astrophys. Suppl. 131, 137 (1998). [6] S Chandra, D A Varshalovich and W H Kegel, Pramana - J. Phys. 25, 557 (1995). [7] S Chandra, Indian J. Phys. 76В, 649 (2002). Pramana - J. Phys., Vol. 62, No.

  20. The Mira Variable S Orionis: Relationships Between the Photosphere, Molecular Layer, Dust Shell, and SiO Maser Shell at 4 Epochs

    Science.gov (United States)

    2007-01-01

    1992; Haniff et al. 1995; van Belle et al. 1996; Thompson et al. 2002; Mennesson et al. 2002; Hofmann et al. 2002; van Belle et al. 2002; Perrin et al...2003, Proc. SPIE, 4838, 89 Gray, M. D., & Humphreys, E. M. L. 2000, New Astron., 5, 155 Haniff , C. A., Scholz, M., & Tuthill, P. G. 1995, MNRAS, 276

  1. A Catalog of Solar White-Light Flares (1859-1982), Including Their Statistical Properties and Associated Emissions.

    Science.gov (United States)

    1983-09-20

    d’eruption solaires en lumiere integrale , Orion 18:403. 9. Fritzova, L. , Kopecky, Al. , and Svestka, Z. (1958) Publ. Astron. Inst. Czech. Acad. Sci...protuberantielle au sein d’une tache solaire, L’Astronomie 36:276. 25. DuMartheray, M. (1948) Observations d’eruptions solaire en lumiere integrale

  2. Kes annab klaverile hinge? / Alo Põldmäe

    Index Scriptorium Estoniae

    Põldmäe, Alo, 1945-

    2010-01-01

    Sihtasutuse Tallinn 2011 koostööpartneri Eesti Rahvusliku Kalverimuuseumi ja Tartu Saksa Kultuuriinstituudi korraldatavast muusikaõhtust "Hingega klaver - ajaloorännakud eesti ja saksa klaveritel". Eesti tiibklaveri Astron ja saksa tiibklaveri C. Bechstein ajaloost, klaverimeister Ernst Hiis'i tegevusest

  3. Why don't clumps of cirrus dust gravitationally collapse?

    NARCIS (Netherlands)

    Schild, R.E; Gibson, C.H.; Nieuwenhuizen, T.M.; Wickramasinghe, N.C.

    2012-01-01

    We consider the Herschel-Planck infrared observations of presumed condensations of interstellar material at a measured temperature of approximately 14 K (Juvela et al 2012 Astron. Astrophys. 541 A12), the triple point temperature of hydrogen. The standard picture is challenged that the material is

  4. Nancay blind 21cm line survey of the Canes Venatici group region

    NARCIS (Netherlands)

    Kraan-Korteweg, R. C.; Driel, W. van; Briggs, F.; Binggeli, B.; Mostefaoui, T. I.

    1998-01-01

    Submitted to: Astron. Astrophys. Abstract: A radio spectroscopic driftscan survey in the 21cm line with the Nancay Radio Telescope of 0.08 steradians of sky in the direction of the constellation Canes Venatici covering a heliocentric velocity range of -350 < V_hel < 2350 km/s produced 53 spectral

  5. Fast Transients with the Square Kilometre Array and its Pathfinders ...

    Indian Academy of Sciences (India)

    The Institute of Mathematical Sciences – HBNI, Tamarani, Chennai 600 113, India. Currently at: ASTRON, Netherlands Institute for Radio Astronomy, Dwingeloo, The Netherlands; Raman Research Institute, C. V. Raman Avenue, Sadashivanagar, Bangalore 560 080, India. Indian Institute of Technology Kharagpur, ...

  6. Proceedings of Colloquium 110 of the International Astronomical Union on Library and Information Services in Astronomy Held in Washington, DC on 26 July- 1 August 1988

    Science.gov (United States)

    1989-01-01

    Netherlands)); Miley, G.K. (Space Telescope Science Inst.. Baltimore, MO (USA)) SO Astron. Astrophys. ( Sep 1988) v. 203(2) p. 250-254 ISSN 0004-6361; CODEN...colleagues. The whole body of accumulated information became universally available. A celebrated example is the famous Historia Coelestis of Tycho Brahe. An

  7. Gravitational lensing statistics with extragalactic surveys; 2, Analysis of the Jodrell Bank-VLA Astrometric Survey

    NARCIS (Netherlands)

    Helbig, P.; Marlow, D. R.; Quast, R.; Wilkinson, P. N.; Browne, I. W. A.; Koopmans, L. V. E.

    1999-01-01

    Published in: Astron. Astrophys. Suppl. Ser. 136 (1999) no. 2, pp.297-305 citations recorded in [Science Citation Index] Abstract: We present constraints on the cosmological constant $lambda_{0}$ from gravitational lensing statistics of the Jodrell Bank-VLA Astrometric Survey (JVAS). Although this

  8. Solar Magnetic Atmospheric Effects on Global Helioseismic ...

    Indian Academy of Sciences (India)

    ematical structure of the model has since inspired many (Evans & Robert 1990,. 1991; Murawski & Roberts 1993b; Jain & Roberts 1991; Tirry et al. 1998; ..... Chaplin, W. J., Elsworth, Y., Isaak, G. R., Lines, R., McLeod, C. P., Miller, B. A., New, R. 1998, Mon. Not. Roy. Astron. Soc., 300, 1077–1090. Chaplin, W. J., Elsworth, Y., ...

  9. Bianchi Type-I, V and VIo models in modified generalized scalar ...

    Indian Academy of Sciences (India)

    2003). [11] R Kantowski and R K Sachs, J. Math. Phys. 7, 443 (1966). [12] P Endo and T Fukui, Gen. Relativ. Gravit. 8, 833 (1977). [13] K Arai, M Hashimoto and T Fukui, Astron. Astrophys. 179, 17 (1987). [14] T Fukui and J M Overduin, Gen. Relativ.

  10. Knowledge Architect : A Tool Suite for Managing Software Architecture Knowledge

    NARCIS (Netherlands)

    Liang, Peng; Jansen, Anton; Avgeriou, Paris

    2009-01-01

    Management of software architecture knowledge (AK) is vital for improving an organization’s architectural capabilities. To support the architecting process within our industrial partner: Astron, the Dutch radio astronomy institute, we implemented the Knowledge Architect (KA): a tool suite for

  11. Spicules Intensity Oscillations in SOT/HINODE Observations E ...

    Indian Academy of Sciences (India)

    2015-04-01

    Apr 1, 2015 ... Phys., 283, 187T. Tavabi, E. 2014, Astrophys. Space Sci., 352, 43T. Tavabi, E., Koutchmy, S., Ajabshirizadeh, A., Ahangarzadeh Maralani, A. R., Zeighami, S. 2014, Astron. Astrophys., arXiv:1409.7654v2[astro-ph.SR] 30 Sep 2014. Trauth, M. H., MATLAB Recipes for Earth Sciences, Second Edition, Chapter ...

  12. Field #3 of the Palomar-Groningen Survey; 1, Variable stars at the edge of the Sagittarius dwarf galaxy

    NARCIS (Netherlands)

    Schultheis, M.

    1996-01-01

    Submitted to: Astron. Astrophys. Abstract: A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 of the Palomar-Groningen Survey, at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with

  13. An electronic submission service for Astronomy and Astrophysics

    NARCIS (Netherlands)

    Hogeveen, S.J.

    1998-01-01

    This paper outlines an Electronic Submission Service (ess) for Astron- omy and Astrophysics, suitable for all parts of the journal: Letters, Main Journal, andSupplements. The proposed service should be run by a pro- fessional entity: one of the publishers, eso, thecds, orsome other, yetto be

  14. Training in Astronomy for Physics Students J. H. Fan1,2

    Indian Academy of Sciences (India)

    telescope for observations and some experiments for their thesis and innova- tion competitions. Some undergraduates received awards issued by the National. Astronomical Observatory of China for their interesting research work in astron- omy. Some students have chosen to do their MSc programme in astrophysics, and.

  15. Results of the ESO-SEST Key Programme on CO in the Magellanic Clouds. IX. The giant LMC HII region complex N11

    NARCIS (Netherlands)

    Israel, F. P.; Graauw, T. de; Johansson, L. E. B.; Booth, R. S.; Boulanger, F.; Garay, G.; Kutner, M. L.; Lequeux, J.; Nyman, L. A. A.; Rubio, M.

    2002-01-01

    Published in: Astron. Astrophys. 401 (2003) 99-112 citations recorded in [Science Citation Index] Abstract: We present maps and a catalogue containing the J=1-0 12CO parameters of 29 individual molecular clouds in the second-brightest LMC star formation complex, N11. In the southwestern part of N11,

  16. En la Biblioteca Luis Ángel Arango. El mapa del Río Magdalena de Humboldt

    Directory of Open Access Journals (Sweden)

    Jorge Arias de Greiff

    1970-06-01

    Full Text Available Humboldt, durante la larga navegación remontando el río de la Magdalena en los meses de abril, mayo y junio de 1801, determinó astronómicamente la ubicación de numerosos lugares.

  17. Galactic Diffuse Polarized Emission Ettore Carretti

    Indian Academy of Sciences (India)

    starting to take shape, but essential points are still under debate, like number and position of reversals or the field pattern in the outer galaxy. The situation in the ..... Wolleben, M., Landecker, T. L., Hovey, G. J., Messing, R., Davison, O. S., House, N. L.,. Somaratne, K. H. M. S., Tashev, I. 2010a, Astron. J., 139, 1681. Wolleben ...

  18. and density-dependent quark mass model

    Indian Academy of Sciences (India)

    659–668. Radial oscillations of magnetized proto strange stars in temperature- and density-dependent quark mass model. V K GUPTA£, ASHA GUPTA, ..... D58, 083001 (1998). [13] O G Benvenuto and G Lugones, Mon. Not. R. Astron. Soc. 304, L25 (1999). [14] V K Gupta, Asha Gupta, S Singh and J D Anand, Int. J. Mod.

  19. Solar Magnetic Flux Ropes Boris Filippov1,∗, Olesya Martsenyuk1 ...

    Indian Academy of Sciences (India)

    2015-01-09

    . Paletou, F., Aulanier, G. 2003, in Solar Polarization Workshop 3, edited by Trujillo Bueno, J.,. Sánchez Almeida, J., CS-236, Astron. Soc. Pac., San Francisco, p. 458. Pariat, E., Antiochos, S. K., DeVore, C. R. 2009, Astrophys.

  20. The Theory of Gamma-Ray Bursts

    Science.gov (United States)

    Dai, Zigao; Daigne, Frédéric; Mészáros, Peter

    2017-10-01

    This chapter gives a brief review on the theory of gamma-ray bursts (GRBs), including the models of multi-messengers (e.g., prompt multiwavelength electromagnetic emissions, high-energy neutrinos, ultra-high-energy cosmic rays, and gravitational waves) and central engines (in particular, mergers of binary neutron stars for short GRBs). For detailed reviews, please see (Piran in Phys. Rep. 314:575, 1999; Rev. Mod. Phys. 76:1143, 2004; Mészáros in Annu. Rev. Astron. Astrophys. 40:137, 2002; Rep. Prog. Phys. 69:2259, 2006; Zhang and Mészáros in Int. J. Mod. Phys. A 19:2385, 2004; Zhang in Chin. J. Astron. Astrophys. 7:1, 2007; Nakar in Phys. Rep. 442:166, 2007; Kumar and Zhang in Phys. Rep. 561:1, 2015).

  1. Evidence of Magnetoacoustic Oscillations above the Brightened and ...

    Indian Academy of Sciences (India)

    A. K. SRIVASTAVA

    2017-11-23

    Nov 23, 2017 ... De Moortel, I., Ireland, J., Hood, A.W., Walsh, R.W. 2002,. Astron. Astrophys., 387, L13. De Pontieu, B., Erdélyi, R., de Wijn, A. G. 2003, Astrophys. J., 595, L63. De Pontieu, B., Tarbell, T., Erdélyi, R. 2003, Astrophys. J.,. 590, 502. De Pontieu, B., Erdélyi, R., James, S. P. 2004, Nature, 430,. 536. De Pontieu, B.

  2. Science and Technology Metrics

    Science.gov (United States)

    2005-01-01

    NOT R ASTRON SOC 232 DIAGNOSTICA 230 REV INT PSICOLOGIA C 227 ASTROPHYS J 2 224 Page 499 PSYCHOTHER PSYCH MED 223 STRATEGIC MANAGE J 221 COUNS PSYCHOL...J; Buela-Casal, G. 2003. Comparative analysis of Health Psychology Page 507 journals published in Spanish. REVISTA LATINOAMERICANA DE PSICOLOGIA 35 (3...Buela-Casal, G. 2003. Comparative analysis of clinical psychology journals published in Spanish. REVISTA MEXICANA DE PSICOLOGIA 20 (1): 141-155. Breunung

  3. Differential Cartography

    Science.gov (United States)

    1992-07-13

    dem Abgebildeten in den kleinsten Theilen ihnlich wird, Astron. Abh. herausgegeben v. H. C. Schumacher, Heft III = Carl Friedrich Gauss Werke, Bd 4...Abh. der Kdnigl. Ges. der Wiss. zu G~ittingen 11 = Carl Friedrich Gauss Werke, Bd. 4, Konigl. Ges der Wiss. zu G~ittingen (1880), 259-3(X). Lagrange...Lagrange (1779) considered the general problem of conformal projections for surfaces of revolution. The term ’conformal’ was introduced by Gauss (1822

  4. NIR observations of V404 Cyg with PANIC

    Science.gov (United States)

    Shaw, A. W.; Knigge, C.; Meisenheimer, K.; Ibanez, J. M.

    2015-07-01

    We report on NIR photometry of the black hole X-ray transient, V404 Cyg during its current outburst (GCN #17929). The source was observed between 27 Jun 22:47 UT - 29 Jun UT 02:28 with the PANoramic Near Infrared Camera (PANIC) on the 2.2m telescope at the Centro Astron & oacute;mico Hispano-Alem & aacute;n (CAHA) on Calar Alto, Spain.

  5. The Method of Eichhorn with Non-Standard Projections for a Single Plate

    Science.gov (United States)

    Cardona, O.; Corona-Galindo, M.

    1990-11-01

    RESUMEN. Se desarrollan las expresiones para el metodo de Eichhorn en astrometria para proyecciones diferentes a la estandar. El se usa para obtener las coordenadas esfericas de estrellas en placas astron6micas cuando las variables contienen errores. ABSTRACT. We develop the expressions for the Eichhorn's Method in astrometry for non-standard projections. The method is used to obtain spherical coordinates of stars in astronomical plates, when all the variables have errors. Key words: ASTROMETRY

  6. Very Large Array Observations of the Sun with Related Observations Using the SMM (Solar Maximum Mission) Satellite

    Science.gov (United States)

    1988-10-12

    longitudinal magnetic field ponds to a longitudinal magnetic field strength of H, = strengths H, % 1800 gauss (n = 3) provided that the 600 gauss...release and source of flare energy (Gold and Hoyle , 1960; Heyvaerts et al., 1977; Rust, 1972, 1976). Recent VLA observations at 6 cm wavelength (Kundu et al...359. * Felli, M., Lang, K. R., and Willson, R. F.: 1981, Astrophys. 1. 247, 325. Gold, T. and Hoyle , F.: 1960, Monthly Notices Roy. Astron. Soc. 8i

  7. Proceedings of the Antiproton Science and Technology Workshop Held in Santa Monica, California on 6-9 October 1987

    Science.gov (United States)

    1988-07-01

    Measurement of the 110 - 1ii Submillimeter Line of H2 D+", Astron. Astrophys. 137(2), L15-6 (1984). 417 ge, PC 47. Lubic, Karen G.; Amano, T., "Observation of...195 (1974). Also see R.G. McQueen , S.P. Marsh, J.W. Taylor, J.N. Fritz, and W.J. Carter, in High-Velocity Impact Phenomena, R. Kinslow, ed

  8. Orbit Determination Performance Improvements for High Area-to-Mass Ratio Space Object Tracking Using an Adaptive Gaussian Mixtures Estimation Algorithm

    Science.gov (United States)

    2009-07-01

    class of orbits, the set of quantities used in hypothesis generation for this work is taken to be: the geocentric range, the velocity magnitude along the...Given a hypothesized geocentric range, r, the inertial position of the object with respect to the geocenter is constructed by first forming the unit...Farinella and F. Mignard, “Solar radiation pressure perturbations for Earth satellites: I. A complete theory including penumbra transitions,” Astron

  9. Los cometas de Atawallpa: acerca del papel de las profecías en la política del Estado Inka

    Directory of Open Access Journals (Sweden)

    Mariusz Ziólkowski

    1988-12-01

    Full Text Available En este artículo quisiera detenerme sólo sobre el eventual impacto que pudieron haber tenido el calendario estatal inca y las profecías basadas  en la interpretación de los fenómenos astronómicos extraordinarios, en la actitud que tomaron los dirigentes del Imperio, y especialmente Atawallpa, frente a los españoles.

  10. Coeficientes de extinción del CASLEO y características del CCD directo con el telescopio JS

    Science.gov (United States)

    Baume, G. L.; Campuzano-Castro, F.; Fernández-Lajús, E.; Gamen, R.; Haucke, M.; Marchesini, E. J.; Molina-Lera, J. A.; Rossignoli, N. L.; San Sebastián, I. L.; Tello Huanca, E. L.; Zanardi, M.

    We computed atmospheric extinction coefficients at the Complejo Astronómico El Leoncito (CASLEO) in UBVRI bands. They were obtained from photometric observations carried out in December 2011 using the 2.15-m ``Jorge Sahade'' Telescope (JS) and we compared then with previous published values. We also computed several instrumental parameters of the ROPER CCD 1300B camera working in direct mode and we presented results of a linearity test. FULL TEXT IN SPANISH

  11. Observando los efectos de la Relatividad General alrededor de los agujeros negros

    OpenAIRE

    Barcons, Xavier

    2015-01-01

    Observaciones astronómicas de la materia que rodea los agujeros negros ponen en evidencia algunas predicciones de la Relatividad General en condiciones de campo gravitatorio fuerte. Una de ellas, el redshift gravitatorio, no solo se observa de forma rutinaria sino que se usa para medir la rotación del agujero negro. El spin de los agujeros negros gigantes encierra la clave de su crecimiento, e indirectamente de la evolución de las galaxias.

  12. Relics as Probes of Galaxy Cluster Mergers R. J. van Weeren1,∗ , M ...

    Indian Academy of Sciences (India)

    Relics as Probes of Galaxy Cluster Mergers. R. J. van Weeren1,∗. , M. Brüggen2, H. J. A. Röttgering1 & M. Hoeft3. 1Leiden Observatory, Leiden University, P.O. .... Jones, F. C., Ellison, D. C. 1991, Space Sci. Rev., 58, 259. Keshet, U. 2010, ArXiv e-prints. Komissarov, S. S., Gubanov, A. G. 1994, Astron. Astrophys., 285, 27.

  13. Astronomía y Física: un matrimonio Sartriano

    Science.gov (United States)

    Vucetich, H.

    Desde el siglo XVII, Física y Astronomía han formado un matrimonio similar al de Sartre y Beauvoir: lleno de amores contingentes, pero firme y duradero. En la charla examino tres de los frutos más recientes de este matrimonio: - La confirmación de la Relatividad General con datos astronómicos. - Astrofísica y Física de neutrinos. - Teorías de supercuerdas y astronomía.

  14. Astronomía en la cultura

    Science.gov (United States)

    López, A.; Giménez Benitez, S.; Fernández, L.

    La Astronomía en la Cultura es el estudio interdisciplinario a nivel global de la astronomía prehistórica, antigua y tradicional, en el marco de su contexto cultural. Esta disciplina abarca cualquier tipo de estudios o líneas de investigación en que se relacione a la astronomía con las ciencias humanas o sociales. En ella se incluyen tanto fuentes escritas, relatos orales como fuentes arqueológicas, abarcando entre otros, los siguientes temas: calendarios, observación práctica, cultos y mitos, representación simbólica de eventos, conceptos y objetos astronómicos, orientación astronómica de tumbas, templos, santuarios y centros urbanos, cosmología tradicional y la aplicación ceremonial de tradiciones astronómicas, la propia historia de la astronomía y la etnoastronomía (Krupp, 1989) (Iwaniszewski, 1994). En nuestro trabajo abordamos la historia y situación actual de esta disciplina, sus métodos y sus relaciones con otras áreas de investigación.

  15. Segundo Catálogo Estelar del Hemisferio Sur con Astrolabio Fotoeléctrico PAII

    Science.gov (United States)

    Manrique, W. T.; Podestá, R. C.; Alonso, E.; Actis, E. V.; Pacheco, A. M.; Bustos, G.; Lizhi, L.; Zezhi, W.; Fanmiao, Z.; Hongqi, W.; Perdomo, R.

    Recordamos que entre el Observatorio Astronómico ``Félix Aguilar'', el Observatorio Astronómico de Beijing y el Observatorio Astronómico de La Plata, se ha convenido en desarrollar un Proyecto de Investigación conjunto, para la observación sistemática de estrellas en el Hemisferio Sur, con el objeto de la elaboración de un Catálogo Estelar Global utilizando un Astrolabio Fotoeléctrico PAII del Observatorio de Beijing, que ha sido usado con éxito en la República de China. En este trabajo se presenta el Segundo Catálogo Estelar del Hemisferio Sur, derivado de las observaciones realizadas con el PAII instalado en el OAFA, durante el períiodo Febrero de 1992 a Marzo de 1997. En este lapso se han observado mas de 400000 pasajes estelares, obteniéndose las correcciones Δ α y Δ δ de 5241 estrellas del FK4, FK5, FK5 Ext., SRS, CAMC y GC. Las precisiones medias son del orden de ± 3,2 ms en ascensión recta y ±0."057 en declinación. Rango de magnitudes : 2,0 a 11,5 Rango de declinaciones : -3o a -60o Epoca Media : 1994.9 Se analizan los residuos en función de la magnitud y tipo espectral, correcciones de grupo y frecuencia de distribución Δ α y Δ δ.

  16. The la Plata Astronomical Data Center

    Science.gov (United States)

    Marraco, H. G.

    1990-11-01

    RESUMEN. El Centro de Datos Astron6micos tiene su sede en la Facuitad de Ciencias Astron6micas y Geofisicas d la Universidad Nacional de La Plata y funciona por convenio entre esta facultad y el Centre des Stellaires de la Universite' Louis Pasteur en Estrasburgo (CDS), Francia. La finalidad de este centro es la de proveer a los astr6nomos del area con copias de los alrededor de 500 acumulados y/o preparados por el CDS a la vez que promover la producci6n y/o acumulaci6n de en el rea. Para la realizaci6n de esta tarea se cuenta con el apoyo del Centro Superior para el Procesamiento de la Informaci6n (CESPI) de la UNLP cuyos equipos se describen. Las tareas que se estan realizando incluyen la distribuci6n de SIMBAD a los astr6nomos argentinos y se efectuan ensayos de distribuci6n en linea de CD-ROM TEST DISK del Astronomical Data Center (ADC) de la NASA que contiene los 31 mas solicitados por los astr6nomos de todo el mundo. ABSTRACl The La Plata Astronomical Data Center operates by an agreement between the Facultad de Ciencias Astron6micas y Geofisicas at La Plata University and the Centre des Donnees Stellaires of Louis Pasteur University at Strasbourg (CDS), France. The purpose of the Center is to provide to the area astronomers with copies of the catalogs they need amongst those stored and/or prepared at CDS. At the same time the center will act of the astronomical data produced within its area. K words: DATA ANALYSIS

  17. Cámara CCD Directa con el Telescopio de 2.15 m del CASLEO: algunos diagnósticos

    Science.gov (United States)

    Cellone, S. A.

    Se efectuaron algunas pruebas con la cámara CCD (+ Reductor Focal) instalada en el foco Cassegrain del Telescopio de 2.15 m del Complejo Astronómico El Leoncito (CASLEO). Las conclusiones más significativas son: Los tiempos de exposición efectivos difieren de los nominales en una fracción apreciable de segundo. En exposiciones de menos de 3 segundos, la iluminación no es pareja en todo el detector. En consecuencia, se recomiendan los pasos a seguir por los astrónomos tanto durante la observación como en la reducción de sus datos.

  18. Microresonator Frequency Comb Optical Clock

    Science.gov (United States)

    2014-07-22

    and T. J. Kippenberg , “Optical frequency comb generation from a monolithic microresonator,” Nature 450, 1214–1217 (2007). 2. T. J. Kippenberg , R...Mon. Not. R. Astron. Soc. 380, 839–847 (2007). 8. P. Del’Haye, O. Arcizet, A. Schliesser, R. Holzwarth, and T. J. Kippenberg , “Full stabilization of a...Lett. 112, 043905 (2014). 18. T. Herr, V. Brasch, J. D. Jost, C. Y. Wang, N. M. Kondratiev, M. L. Gorodetsky, and T. J. Kippenberg , “Temporal solitons

  19. Precision Narrow-Angle Astrometry of Binary Stars with the Navy Prototype Optical Interferometer

    Science.gov (United States)

    2004-01-01

    catalogs include the Washington Double Star Catalog,5 the Sixth Orbit Catalog,6 the Eighth Spectroscopic Binary Catalog,7 and the Bright Star Catalog...the Navy. This research has made use of the Washington Double Star Catalog, maintained at the U.S. Naval Observatory, and of the SIMBAD database... star CD-ROM. I. The Washington Double Star Catalog,” Astron. J. 122, pp. 3466– 3471 (see also http://ad.usno.navy.mil/wds/wds.html), 2001. 6. W. I

  20. Astrogeodynamic Studies of Latitude Variations during the period: 1992-2002

    Science.gov (United States)

    Alonso, E.; Pacheco, A.; Podesta, R.; Actis, E.

    2006-06-01

    Astrogeodynamics is a growing activity in astronomical research. Observatorio Astronómico Félix Aguilar takes part of it by means of Photoelectric Astrolabe PA 2 observations from San Juan, Argentina. Here we present a comparison between Instantaneous Latitude Variation and data published by IERS, for the period February 1992 to December 2002. The resulting curve has been obtained from observations of the Fundamental Stars Groups, computing weight values of Latitude Variation for each night, previously corrected for Pole Movement. Finally we analyze the possibility of a relation between this curve and the occurrence of earthquakes of more than 5 magnitudes (Mercalli scale).

  1. Formación de los planetas gigantes del Sistema Solar

    OpenAIRE

    Guilera, Octavio Miguel

    2014-01-01

    El estudio de los sistemas planetarios es uno de los temas fundamentales de las ciencias astronómicas. El interés en nuestro Sistema Solar surgió en tiempos remotos. Hace casi dos décadas, Mayor y Queloz (1995) detectaron el primer planeta extrasolar en órbita alrededor de una estrella de tipo solar. Este notable descubrimiento ha hecho surgir desde entonces un enorme interés en el estudio de sistemas planetarios en general. Esta Tesis es una continuación natural de un proyecto de i...

  2. Abandoned Paleocene spreading center in the northeastern Indian Ocean: evidence from magnetic and seismic reflection data

    Digital Repository Service at National Institute of Oceanography (India)

    Krishna, K.S.; Rao, D.G.

    Dorsales de l’Ocean Indien par les Methods dela Cinematique des Plaques. Territoires des Terres Australes et Antarctique Francaises, Paris, 308 pp. Pierce, J.W., 1978. The northward motion of India since the Late Cretaceous. R. Astron. Soc., Geophys. J. 52... Fracture Zone FZ and the 908E FZ Sclater and Fisher, 1974; Peirce, . 1978; Royer et al., 1991; Krishna et al., 1995 are ) Corresponding author. E-mail: krishna@csnio.ren.nic.in poorly constrained. To address this shortfall, mag- netic data in the region...

  3. Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009

    Science.gov (United States)

    2011-01-01

    Mech. 29, 309–321 (1983) Davies, M.E., Abalakin, V.K., Bursa , M., Lederle, T., Lieske, J.H., Rapp, R.H., Seidelmann, P.K., Sinclair, A.T., Teifel...Celest. Mech. 39, 103–113 (1986) Davies, M.E., Abalakin, V.K., Bursa , M., Hunt, G.E., Lieske, J.H., Morando, B., Rapp, R.H., Seidelmann, P.K...1988. Celest. Mech. Dyn. Astron. 46, 187–204 (1989) Davies, M.E., Abalakin, V.K., Brahic, A., Bursa , M., Chovitz, B.H., Lieske, J.H., Seidelmann

  4. Raízes pós-mitológicas da Astronomia Clássica

    Science.gov (United States)

    di Bartolo, L.; Villas da Rocha, J. F.

    2004-02-01

    Apresentamos como a invenção de um modelo astronômico e cosmológico fundado em causas naturais foi um processo gestado num ambiente cultural específico, o do advento do pensamento pós-mitológico, que tem como sua raiz mais funda a trajetória particular da Grécia Antiga, com ênfase na resolução de uma grave crise social e a evolução do mundo clássico para o contexto espiritual de um império universal.

  5. Educación no formal

    Science.gov (United States)

    Tignanelli, H.

    Se comentan en esta comunicación, las principales contribuciones realizadas en el campo de la educación en astronomía en los niveles primario, secundario y terciario, como punto de partida para la discusión de la actual inserción de los contenidos astronómicos en los nuevos contenidos curriculares de la EGB - Educación General Básica- y Polimodal, de la Reforma Educativa. En particular, se discuten los alcances de la educación formal y no formal, su importancia para la capacitación de profesores y maestros, y perspectivas a futuro.

  6. Ondas gravitacionales de choque

    OpenAIRE

    Ranea Sandoval, Ignacio Francisco

    2010-01-01

    En este trabajo monográfico se presenta un breve resumen relacionado con las ondas gravitacionales y con la teoría general de la relatividad. Realizado esto se presenta una adaptación de trabajos científicos asociados con un fenómeno conocido como ondas gravitacionales de choque. Trabajo final de Introducción a la Astrofísica de Agujeros Negros. Facultad de Ciencias Astronómicas y Geofísicas

  7. Gravitational Rutherford scattering and Keplerian orbits for electrically charged bodies in heterotic string theory

    Science.gov (United States)

    Villanueva, J. R.; Olivares, Marco

    2015-11-01

    Properties of the motion of electrically charged particles in the background of the Gibbons-Maeda-Garfinkle-Horowitz-Strominger black hole is presented in this paper. Radial and angular motions are studied analytically for different values of the fundamental parameter. Therefore, gravitational Rutherford scattering and Keplerian orbits are analyzed in detail. Finally, this paper complements previous work by Fernando for null geodesics (Phys Rev D 85:024033, 2012), Olivares and Villanueva (Eur Phys J C 73:2659, 2013) and Blaga (Automat Comp Appl Math 22:41-48, 2013; Serb Astron 190:41, 2015) for time-like geodesics.

  8. La gravedad en Bruno, Kleper y Newton. la distribución de la materia y sus implicaciones cosmológicas

    OpenAIRE

    M. Diego Pintado

    2016-01-01

    En este trabajo se describe en modo sucinto el papel fundamental y determinante del problema de la gravitación universal en la historia de la cosmología moderna, indagándose así mismo los factores que le dieron origen, principalmente la proposición de la formulación de la ley de gravedad, sus antecedentes, y a su vez se repasan los problemas astrofísicos, astronómicos y filosóficos de este nuevo esquema cosmológico. El esquema de esta monografía traza un breve examen epistemológico, luego un ...

  9. O imaginário extraterrestre na cultura portuguesa : do fim da Modernidade até meados do séc. XIX

    OpenAIRE

    Conceição, Joaquim Fernandes da

    2004-01-01

    Procede-se a uma inventariação de fontes de diverso teor que refiram ideias, conceitos e representações cosmológicas e astronómicas, especificamente conotadas com o âmbito "extraterrestre" e as noções sobre o Outro não terrestre e porventura não-humano. Analisa-se a rede de influências, mormente de leituras, que possam ter determinado as opções dos nossos mentores culturais sobre o tema.

  10. Evolution of Timescales from Astronomy to Physical Metrology

    Science.gov (United States)

    2011-07-20

    the BIH changed its procedure to use only the three standards located at the US National Bureau of Standards, the Swiss Laboratoire Suisse de...Giacomo P 1981 News from the BIPM Metrologia 17 69–74 [32] Arias E F, Panfilo G and Petit G 2011 Metrologia 48 S145–53 [33] Müller E A and Jappel A (ed...Standish E M 1998 Time scales in the JPL and CfA ephemerides Astron. Astrophys. 335 381–4 [38] Petit G 2000 Use of primary frequency standards for estimating

  11. Adventures in order and chaos : a scientific autobiography

    Science.gov (United States)

    Contopoulos, George

    The field of Order and Chaos had a remarkable expansion in the last 50 years. The main reason was the use of computers, and the development of new theoretical methods that we call now 'the theory of chaos'. The author describes this fascinating period in a relaxed and sometimes humorous autobiographical way. He relates his interactions with many people in dynamical astronomy and he quotes several anecdotes from these interactions. He refers also to his experiences when he served in various international positions, such as general secretary of the IAU and chairman of the journal Astronomy and Astrophysics. In recent years the theory of chaos has been extended to new areas, like relativity, cosmology and quantum mechanics and it continues expanding in almost all branches of physics. The book describes many important ideas in this field in a simple way. It refers also to problems of more general interest, like writing papers and giving lectures and the interaction of authors and referees. Finally it gives some useful prospects for the future of dynamical astronomy and related fields. George Contopoulos, PhD U.Athens1953; Professor of Astronomy U.Thessaloniki 1957-75; U.Athens 1975-96; Emeritus 1996-; Member, Academy of Athens 1997-. Visiting Professor Yale U., Harvard U., MIT, Cornell U., U.Chicago, U.Maryland, U. Florida, Florida State U., U. Milan; Res. Associate, Yerkes Obs., Inst.Adv.Study Princeton, Inst.Space Studies, Goddard Flight Center, Columbia U., ESO. Author or Editor of 15 books, and about 250 papers on Galactic Dynamics, Relativity and Celestial Mechanics. Positions held: Gen.Secretary of the IAU; Director General Nat.Obs.of Greece, Pres.Hellenic Astron.Soc.; Nat.Representative of Greece in NATO, etc. Distinctions: Amer. Astron.Soc. Brouwer Prize; U.Chicago, Honorary Doctor's Degree; IAU, Pres. Commission 33 (Galaxy); Member Academia Europaea; Associate Royal Astron. Soc.; Chairman of the European Journal "Astronomy and Astrophysics"; Assoc. Editor of

  12. Eventos Planetarios Periodicos

    Science.gov (United States)

    Flores Gutierrez, J. D.

    1987-05-01

    El análisis de las coordenadas ecuatoriales para los planetas Mercurio, Venus, Marte, Júpiter, Saturno, en los instantes en que ocurren algunos eventos astronómicos, como conjunciones, oposiciones,etc., muestra un comportamiento periódico, característico a cada planeta. El caso de Venus es el mejor estudiado. El cálculo de las efemérides a lo largo de 1000 años , indica un período característico de aproximadamente 260 años. Resultados preliminares con otros planetas muestran períodos distintos.

  13. Comportamiento de la cromósfera solar en la línea H-alfa durante el período enero/05-agosto/06

    Science.gov (United States)

    Missio, H.; Davoli, D.; Aquilano, R.

    Using the instrument at Observatorio Astronómico Municipal de Rosario (OAMR), we analyze the solar chromospheric activity during the period January/05-August/06. The instrument is a Carl Zeiss refractor telescope of 150 mm aperture and 2250 mm of focal distance with a monochromatic filter in the H-alpha line. We take as proxy for the solar activity the area covered by chromospheric ``plages''. The measurements are done using photographic registers. We describe our technique and the results obtained. We observe a decrease of solar activity that corresponds to the end of cycle 23. FULL TEXT IN SPANISH

  14. La arquitectura y el diseño de exhibiciones en el Museo de La Plata

    OpenAIRE

    Inacio, María Alejandra

    2010-01-01

    El Museo se constituye en una pieza esencial, hito cultural y urbano, diseñado y construido ex profeso para serlo, cuyo emplazamiento también era una alegoría ya que se ubica en el Parque de la Ciudad integrándose con el Jardín Zoológico, el Observatorio Astronómico y la Escuela de Bellas Artes y Oficios. Entre 1884-1887 el Museo fue construido con una arquitectura monumental y clásica que imitaba el ideal del Museo Británico. Tímpano, frontis y amplias columnas fueron los elementos simból...

  15. Actividad cromosférica en estrellas frías

    Science.gov (United States)

    Ibañez Bustos, R. V.; Flores, M. G.; Mauas, P. J. D.; Buccino, A. P.

    2017-10-01

    The magnetic fields that cause stellar activity, are generated by the interaction between the convection and stellar rotation (stellar dynamo). In cooler stars, convection becomes dominant. It has been reported that late-type dM stars, even the purely convective ones, present higher levels of activity than those found for the earliest stars. In this article, we present the mean level of activity and variability of a set of eight dM stars from the observations obtained under the HK Project, which operates in the Complejo Astronómico El Leoncito (CASLEO) since 1999.

  16. Establecimiento de una red local en la zona de Tacurú Pucú (Presa de Itaipu- Paraguay)

    OpenAIRE

    Herrera Mérida, Cristina

    2012-01-01

    Este proyecto se enmarca dentro de los trabajos realizados para el Parque Tecnológico Itaipu. La misión principal, dentro de la beca, fue la realización de un proyecto de ingeniería que ayudase en alguno de sus proyectos al PTI. En este sentido se decidió la realización de este proyecto para el posterior empleo de la red local como apoyo en los trabajo de construcción de la nueva sede del PTI-PY, que actualmente ya se están desarrollando. En Paraguay todos los datos y trabajos astronómicos, g...

  17. Finite element modeling methods for photonics

    CERN Document Server

    Rahman, B M Azizur

    2013-01-01

    The term photonics can be used loosely to refer to a vast array of components, devices, and technologies that in some way involve manipulation of light. One of the most powerful numerical approaches available to engineers developing photonic components and devices is the Finite Element Method (FEM), which can be used to model and simulate such components/devices and analyze how they will behave in response to various outside influences. This resource provides a comprehensive description of the formulation and applications of FEM in photonics applications ranging from telecommunications, astron

  18. Anisotropic stars obeying Chaplygin equation of state

    Science.gov (United States)

    Bhar, P.; Govender, M.; Sharma, R.

    2018-01-01

    In this work we provide a framework for modelling compact stars in which the interior matter distribution obeys a generalised Chaplygin equation of state. The interior geometry of the stellar object is described by a spherically symmetric line element which is simultaneously co-moving and isotropic with the exterior space-time being vacuum. We are able to integrate the Einstein field equations and present closed form solutions which adequately describe compact strange star candidates such as 4U 1538-52, PSR J1614-2230, Vela X-1 and Cen X-3 (Gangopadhyay et al, Mon. Not. R. Astron. Soc. 431, 3216 (2013)).

  19. Tidal Mechanism as an Impossible Cause of the Observed Secular Increase of the Astronomical Unit

    Science.gov (United States)

    Itoh, Yousuke

    2009-12-01

    Krasinsky and Brumberg (2004, Celest. Mech. Dyn. Astron., 90, 267) reported a secular increase in the Astronomical Unit ( AU ) of 15 meters per century. Recently, Miura et al. (2009, PASJ, 61, 1247) proposed that angular-momentum transfer from the rotation of the Sun to the orbital motion of the solar-system planets may explain the observed increase of the AU . They assumed that the tidal effect between the planets and the Sun is the cause of this transfer. Here, we claim that a tidal effect cannot be a cause of this type of transfer to explain the increase of the AU .

  20. Ecuaciones diferenciales parciales

    OpenAIRE

    Giordano, Claudia Marcela

    2016-01-01

    El texto reúne los contenidos del curso semestral Ecuaciones Diferenciales Parciales que se dicta desde agosto de 2002 en la Facultad de Ciencias Astronómicas y Geofísicas de la UNLP para alumnos avanzados. Se requiere por parte del lector de una formación básica sobre Análisis Matemático en una y varias variables reales y en variable compleja, así como sobre Álgebra y Álgebra Lineal. Se halla organizado en ocho capítulos, y seis apéndices que incluyen material complementario. En estas not...

  1. Theory and simulation of the optical response of novel nanomaterials from visible to terahertz

    OpenAIRE

    Poyli, Mohamed Ameen

    2015-01-01

    Los avances tecnológicos ocurridos a partir del siglo XVI han permitido explorar tanto el mundo microscópico como el macroscópico, gracias al desarrollo de dispositivos basados en lentes y espejos, desconocidos hasta entonces. El telescopio, inventado por Hans Lippershey y utilizado por Galileo Galilei y sus contemporáneos para realizar sus observaciones astronómicas, ha permitido revelar los misterios del cosmos. En la escala opuesta, el uso del microscopio por Zacharias Janssen, Rober...

  2. CAN GFS GLOBAL FORECASTS BE USEFUL FOR ASTRONOMERS?

    OpenAIRE

    Marín, J. C.; Chacón, A.; Curé, M.

    2011-01-01

    Varios observatorios astronómicos operan actualmente en Chile. Estos necesitan pronósticos atmosféricos exactos con días de anticipación para optimizar la planificación de observaciones y reducir costos de operación. El modelo GFS (Global Forecast System) produce pronósticos atmosféricos cuatro veces al día y sus salidas están disponibles gratis en internet. En este trabajo se presentan resultados preliminares de la estimación y pronóstico de propiedades atmosféricas en los observatorios APEX...

  3. Solar Flare Studies

    Science.gov (United States)

    1982-03-20

    M., Huber, M. C. E. and Timothy, 1. G.: 1977;Appl. Optics 16, 837. Samain, 0., Bonnet , R.M., Gayr’t, R. and Lizambert, C.: 1975, Astron. Astrophys. 39...Simain, D.. Bonnet , R. M., Galet, R., and Lizanbert, G.: 1975,Astr. Atstlophys. 39, 71. Solar.Genphysical Data: 1971, No. 355 Part II. Wlhite, 0. k.: 1964...typically unity, within a factor of two. Acknowledgements We wish to thank those who contributed to the data reduction: Marc Allen and Dennis Ruff at

  4. Herramientas libres para modelar software Free tools to model software

    Directory of Open Access Journals (Sweden)

    Mauro Callejas Cuervo Óscar Yovany Baquero Moreno

    2010-11-01

    Full Text Available Observación acerca del  software libre y de suimplicación en procesos de desarrollo de  softwarecon herramientas 4G por parte de entidades opersonas sin capitales astronómicos y sin lamentalidad acaparadora de dominar el mercado conproductos costosos que las hagan multimillonarias yque no ofrecen una garantía real, ni la posibilidadsiquiera de conocer el  software por el que se hapagado, y mucho menos de modificarlo si no cumplenuestras expectativas.

  5. Gravitational Rutherford scattering and Keplerian orbits for electrically charged bodies in heterotic string theory

    Energy Technology Data Exchange (ETDEWEB)

    Villanueva, J.R. [Universidad de Valparaiso, Instituto de Fisica y Astronomia, Valparaiso (Chile); Centro de Astrofisica de Valparaiso, Valparaiso (Chile); Olivares, Marco [Universidad Diego Portales, Avenida Ejercito Libertador 441, Facultad de Ingenieria, Santiago (Chile)

    2015-11-15

    Properties of the motion of electrically charged particles in the background of the Gibbons-Maeda-Garfinkle-Horowitz-Strominger black hole is presented in this paper. Radial and angular motions are studied analytically for different values of the fundamental parameter. Therefore, gravitational Rutherford scattering and Keplerian orbits are analyzed in detail. Finally, this paper complements previous work by Fernando for null geodesics (Phys Rev D 85:024033, 2012), Olivares and Villanueva (Eur Phys J C 73:2659, 2013) and Blaga (Automat Comp Appl Math 22:41-48, 2013; Serb Astron 190:41, 2015) for time-like geodesics. (orig.)

  6. Gravitational Rutherford scattering and Keplerian orbits for electrically charged bodies in heterotic string theory

    Energy Technology Data Exchange (ETDEWEB)

    Villanueva, J. R., E-mail: jose.villanuevalob@uv.cl [Instituto de Física y Astronomía, Universidad de Valparaíso, Gran Bretaña 1111, Valparaíso (Chile); Centro de Astrofísica de Valparaíso, Gran Bretaña 1111, Playa Ancha, Valparaíso (Chile); Olivares, Marco, E-mail: marco.olivaresr@mail.udp.cl [Facultad de Ingeniería, Universidad Diego Portales, Avenida Ejército Libertador 441, Casilla 298–V, Santiago (Chile)

    2015-11-27

    Properties of the motion of electrically charged particles in the background of the Gibbons–Maeda–Garfinkle–Horowitz–Strominger black hole is presented in this paper. Radial and angular motions are studied analytically for different values of the fundamental parameter. Therefore, gravitational Rutherford scattering and Keplerian orbits are analyzed in detail. Finally, this paper complements previous work by Fernando for null geodesics (Phys Rev D 85:024033, 2012), Olivares and Villanueva (Eur Phys J C 73:2659, 2013) and Blaga (Automat Comp Appl Math 22:41–48, 2013; Serb Astron 190:41, 2015) for time-like geodesics.

  7. COATLI: an all-sky robotic optical imager with 0.3 arcsec image quality

    OpenAIRE

    Watson, Alan M.; Cardona, Salvador Cuevas; Núñez, Luis C. Álvarez; Ángeles, Fernando; Becerra-Godínez, Rosa L.; Chapa, Oscar; Farah, Alejandro S.; Fuentes-Fernández, Jorge; Figueroa, Liliana; Lebre, Rosalía Langarica; Quirós, Fernando; Román-Zúñiga, Carlos G.; Ruíz-Diáz-Soto, Jaime; Tejada, Carlos G.; Tinoco, Silvio J.

    2016-01-01

    COATLI will provide 0.3 arcsec FWHM images from 550 to 900 nm over a large fraction of the sky. It consists of a robotic 50-cm telescope with a diffraction-limited fast-guiding imager. Since the telescope is small, fast guiding will provide diffraction-limited image quality over a field of at least 1 arcmin and with coverage of a large fraction of the sky, even in relatively poor seeing. The COATLI telescope will be installed at the at the Observatorio Astron\\'omico Nacional in Sierra San Ped...

  8. Deployable Camera (DCAM3) System for Observation of Hayabusa2 Impact Experiment

    Science.gov (United States)

    Sawada, Hirotaka; Ogawa, Kazunori; Shirai, Kei; Kimura, Shinichi; Hiromori, Yuichi; Mimasu, Yuya

    2017-07-01

    An asteroid exploration probe "Hayabusa2", that was developed by Japan Aerospace Exploration Agency (JAXA), was launched on December 3rd, 2014 to challenge complicated and accurate operations during the mission phase around the C-type asteroid 162137 Ryugu (1999 JU3) (Tsuda et al. in Acta Astron. 91:356-362, 2013). An impact experiment on a surface of the asteroid will be conducted using the Small Carry-on Impactor (SCI) system, which will be the world's first artificial crater creation experiment on asteroids (Saiki et al. in Proc. International Astronautical Congress, IAC-12.A3.4.8, 2012, Acta Astron. 84:227-236, 2013a; Proc. International Symposium on Space Technology and Science, 2013b). We developed a new micro Deployable CAMera (DCAM3) system for remote observations of the impact phenomenon applying our conventional DCAM technology that is one of the smallest probes in space missions and gained a great success in past Japanese mission IKAROS (Interplanetary Kite-craft Accelerated by Radiation Of the Sun). DCAM3 is a miniaturized separable unit that contains two cameras and radio communication devices for transmission image data to the mothership "Hayabusa2", and it observes the impact experiment at an unsafe region in where the "Hayabusa2" is difficult to stay because of a risk of exploding and impacting debris hitting. In this paper, we report details of the DCAM3 system and development results as well as our mission plan for the DCAM3 observation during the SCI experiment.

  9. The effect of accelerated ageing on colour stability of visible light-cured (VLC) chairside denture liners.

    Science.gov (United States)

    Kostoulas, Ioannis; Polyzois, Gregory; Mitsoudis, Anastasios; Kavoura, Victoria; Frangou, Maria

    2012-06-01

    The purpose of this study was to assess the colour stability of seven visible light-cured (VLC) hard and soft denture liners by an in vitro accelerated ageing test and compare them with two autopolymerised hard and soft liners. Ten specimens of each material were fabricated. The initial colour was measured with a tri-stimulus colorimeter. One set of five specimens was placed in distilled water at 37°C in the dark for 15 days, while the remaining were subjected to UV/visible light-accelerated ageing initially for 24 h and then for 144 h. Colour change (ΔΕ) was calculated. Data were statistically analysed by anova, Tukey and t-tests at α = 0.05. All the liners showed clinically acceptable colour change (ΔΕ ≤ 6.8) in distilled water. The colour changes after ageing for Triad DuaLine, Lightdon U, Ufi Gel H and Light Liner Hard were clinically unacceptable (ΔΕ ≥ 6.8), whereas LightLiner Soft, Astron LC Soft, Triad Resiline and Flexacryl Soft presented slighter and clinically acceptable colour change (ΔΕ ≤ 6.8). Accelerated ageing affected significantly the colour stability of all denture liners tested except Astron LC Soft. Soft VLC denture liners were more colour-stable than hard VLC liners. © 2011 The Gerodontology Society and John Wiley & Sons A/S.

  10. Ajuste de parámetros libres en teorías de campos camaleones a partir de espectros de nubes moleculares galácticas y experimentos terrestres

    Science.gov (United States)

    Teppa Pannia, F. A.; Landau, S. J.

    Resultados recientes, basados en el análisis de espectros moleculares de nubes galácticas a través del método del amoníaco, han arrojado nuevos límites sobre la variación del parámetro adimensional μ=m_e /m_p. Los resultados indican Δ μ/μ = (μ_{obs}-μ_{lab})/μ_{lab}= (2.2± 0.4_{est} ±0.3_{sist}) times 10 ^{-8}, en acuerdo con una variación no nula de dicha cantidad (Levshakov et al. 2010). En este trabajo, motivado por los datos astronómicos, estudiamos la solución lineal del modelo teórico fenomenológico de campo escalar camaleón, presentado por Mota y Shaw (2007), que predice variaciones en μ. Con el fin de cotejar estas predicciones con los resultados observacionales, utilizamos datos de experimentos terrestres que testean violaciones al Principio de Equivalencia para analizar el valor de los parámetros libres presentes en el modelo. El trabajo realizado muestra que la solución estudiada no se puede ajustar a los datos experimentales, sugiriendo que el modelo lineal debe ser descartado para explicar las observaciones astronómicas. FULL TEXT IN SPANISH

  11. New cases of unusual polarimetric behavior in asteroids

    Science.gov (United States)

    Gil-Hutton, R.; Mesa, V.; Cellino, A.; Bendjoya, P.; Peñaloza, L.; Lovos, F.

    2008-04-01

    Aims: Results of different polarimetric campaigns at Complejo Astronómico El Leoncito (Casleo), San Juan, Argentina are presented. The aim of these campaigns was to search for objects exhibiting anomalous polarimetric properties, similar to those shown by the Ld-class asteroid (234) Barbara, among members of the same or similar taxonomic classes. Methods: The data have been obtained with Torino and CASPROF polarimeters at the 2.15 m telescope. The Torino polarimeter is an instrument that allows simultaneous measurement of polarization in five different bands, and CASPROF polarimeter is a two-hole aperture polarimeter with rapid modulation. Results: The campaigns began in 2005, and we found four new asteroids with Barbara-like polarimetric properties: the L-class objects (172) Baucis, (236) Honoria and (980) Anacostia, and the K-class asteroid (679) Pax. The polarimetric properties of the phase-polarization curves of these objects may be produced by a mixture of high- and low-albedo particles in their regolith as a result of the fragmentation of a substrate that is spectrally analog to the CO3/CV3 chondrites. Based on observations carried out at the Complejo Astronómico El Leoncito, operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina and the National Universities of La Plata, Córdoba, and San Juan.

  12. Polarimetric observations of Hungaria asteroids

    Science.gov (United States)

    Gil-Hutton, R.; Lazzaro, D.; Benavidez, P.

    2007-06-01

    Aims:We present the results of a polarimetric program at Complejo Astronómico El Leoncito (Casleo), San Juan, Argentina. The aim of this campaign is to estimate the polarimetric properties of asteroids belonging to the Hungaria dynamical group. Methods: The data were obtained with the Casprof polarimeter at the 2.15 m telescope. The Casprof polarimeter is a two-hole aperture polarimeter with rapid modulation. The campaign began in 2000, and data on a sample of 24 members of the Hungaria group were obtained. We use the slope - albedo or P_min - albedo relationships to get polarimetric albedos for 18 of these objects. Results: Only two Xe-type objects, 434 Hungaria and 3447 Burkhalter, shown a polarimetric behavior compatible with a high albedo object. The A-type asteroid 1600 Vyssotsky has a polarimetric behavior similar to what was observed by Fornasier et al. (2006) for 863 Benkolea, and four objects show P_min values consistent with dark surfaces. Based on observations carried out at the Complejo Astronómico El Leoncito, operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina and the National Universities of La Plata, Córdoba, and San Juan.

  13. Shrinking of Binaries in a WIMPY Background at the Galactic Center

    Science.gov (United States)

    Hills, J. G.

    2001-12-01

    The nature of the dark matter in the Galactic Halo is still not clear. Constraints can be placed on it; e.g., it cannot be in baryons less massive than about 1022 grams (Hills, 1986, Astron. J. 92, 595). It may be in elementary weakly interacting massive particles, WIMPS. Apart from providing most of the mass of the Galaxy, the only known significant dynamical effect of WIMPS is to cause a gradual shrinking of tightly bound binaries (Hills 1983, Astron. J. 88, 1269) as they interact with the background soup of WIMPS. This effect may be observable in binaries close to the Galactic Center if a significant fraction of the mass density near the central black hole is from WIMPS. The requisite binaries would have to have orbital velocities greater than the local velocity dispersion of the WIMPS relative to the binary. The velocity dispersion increases near the black hole. The binary cannot be too close to the black hole or its tidal field will breakup the binary. If the local WIMP density is 107 g/cm3, the fractional rate of reduction in the binary orbital period is about 5 x 10-10/yr for a binary having a semimajor axis equal to 3 solar radii in a soup of WIMPS having a velocity dispersion of 200 km/s relative to the binary. This gradual erosion of the binary period may be detectable, particularly, if one of the binary components is a pulsar.

  14. Laboratory Observation of Instabilities in Stratified Taylor-Couette Flow

    Science.gov (United States)

    Rodenborn, Bruce; Ibanez, Ruy; Swinney, Harry L.

    2015-11-01

    In 2001 Molemaker et al. (J. Fluid. Mech. 448, 1) predicted a new class of instabilities in a system of concentric rotating cylinders that contains a fluid with a vertically varying density. Dubrulle et al. (Astron. Astrophys. 429, 1, 2005) then showed that this phenomenon, which they named stratorotational instability (SRI), could be a source of instability and angular momentum transport in astrophysical accretion disks. Subsequent work by Shalybkov and Rüdiger (Astron. Astrophys. 438, 411, 2005) hypothesized that such stratified flow is stable when the ratio of outer and inner cylinder rotation rates μ is less than the ratio of the inner and outer cylinder radii η. Previous laboratory measurements by Le Bars and Le Gal (Phys. Rev. Lett. 99, 064502, 2007) confirmed this prediction for Re η when the density gradient is large. We also find that the onset of SRI is suppressed for Reynolds numbers Re > 4000 , a region previously unexplored in experiments. For Re > 8000 , we find that the fluid does not exhibit SRI but transitions to a previously unreported chaotic state that mixes the fluid.

  15. On the dark matter as a geometric effect in f (R) gravity

    Science.gov (United States)

    Usman, Muhammad

    2016-11-01

    A mysterious type of matter is supposed to exist because the observed rotational velocity curves of particles moving around the galactic center and the expected rotational velocity curves do not match. This type of matter is called dark matter. There are also a number of proposals in the modified gravity which are alternatives to the dark matter. In this contrast, in 2008, Christian G. Böhmer, Tiberiu Harko and Francisco S.N. Lobo presented an interesting idea in Böhmer et al. (Astropart Phys 29(6):386-392, 2008) where they showed that a f (R) gravity model could actually explain dark matter to be a geometric effect only. They solved the gravitational field equations in vacuum using generic f (R) gravity model for constant velocity regions (i.e. dark matter regions around the galaxy). They found that the resulting modifications in the Einstein Hilbert Lagrangian is of the form R^{1+m}, where m=V_{tg}^2/c^2; V_{tg} being the tangential velocity of the test particle moving around the galaxy in the dark matter regions and c being the speed of light. From observations it is known that m≈ O(10^{-6}) (Böhmer et al. 2008; Salucci et al. in Mon Not R Astron Soc 378(1):41-47, 2007; Persic et al. in Mon Not R Astron Soc 281:27-47, 1996; Borriello and Salucci in Mon Not R Astron Soc 323(2):285-292, 2001). In this article, we perform two things (1) We show that the form of f (R) they claimed is not correct. In doing the calculations, we found that when the radial component of the metric for constant velocity regions is a constant then the exact solutions for f (R) obtained is of the form of R^{1-α } which corresponds to a negative correction rather than positive claimed by the authors of Böhmer et al. (2008), where α is the function of m. (2) We also show that we can not have an analytic solution of f(R) for all values of tangential velocity including the observed value of tangential velocity 200-300 km/s (Salucci et al. 2007; Persic et al. 1996; Borriello and Salucci

  16. Can Ecliptic Comets Be Created En Route from the Kuiper Belt?

    Science.gov (United States)

    (Luke) Dones, Henry C.; Womack, Maria; Nesvorny, David; Bierhaus, Edward B.; Zahnle, Kevin; Robbins, Stuart J.; Bottke, William; Alvarellos, Jose; Hamill, Patrick

    2017-10-01

    The Kuiper Belt is thought to be the reservoir of ecliptic comets (ECs), which include the Jupiter-family comets (JFCs) and Centaurs. ECs are also the main source of Sun-orbiting impactors on the regular moons of the giant planets (Zahnle et al. 2003). Ironically, we still do not know whether the belt, specifically its Scattered Disk, provides enough ECs (Volk and Malhotra 2008). We are investigating whether cometary breakup in the planetary region (Fernández 2009) can substantially increase the number of ECs. In support of this idea, the Kreutz sungrazers may derive from a hierarchical series of fragmentation events of a progenitor long-period comet (e.g., Sekanina and Chodas 2007), and the JFCs 42P and 53P appear to be fragments of a comet that split in 1845 (Kresák et al. 1984). On the other hand, although 16P was tidally disrupted by Jupiter in 1886, only one fragment survives.Models of the cometary orbital distribution ignore activity or apply a physical lifetime based on the number of passages within 2 or 3 AU of the Sun, where sublimation of water ice occurs (Nesvorný et al. 2017). In reality, some comets (e.g., 29P, Hale-Bopp) are active beyond Jupiter due to volatiles such as CO and CO2 (Womack et al. 2017). 174P/Echeclus underwent a 7-magnitude outburst at 13 AU (Rousselot et al. 2016), and CO emission was detected from Echeclus at 6 AU (Wierzchos et al. 2017). We will estimate how the number and size distribution of comet nuclei change with distance from the Sun due to cometary activity and spontaneous disruption, tidal disruption by a giant planet, and tidal disruption of binaries (Fraser et al. 2017).We thank the Cassini Data Analysis Program for support.Fernández Y (2009). Planet. Space. Sci. 57, 1218.Fraser WC, et al. (2017). Nat. Astron. 1, 0088.Kresák L, et al. (1984). IAU Circular 3940.Nesvorný D, et al. (2017). arXiv:1706.07447.Rousselot P, et al. (2016). MNRAS 462, S432.Sekanina, Z, Chodas, PW (2007). Astrophys. J. 663, 657.Volk K

  17. Constraints on the Bulk Composition of Uranus from Herschel PACS and ISO LWS Photometry, SOFIA FORCAST Photometry and Spectroscopy, and Ground-Based Photometry of its Thermal Emission

    Science.gov (United States)

    Orton, Glenn; Mueller, Thomas; Burgdorf, Martin; Fletcher, Leigh; de Pater, Imke; Atreya, Sushil; Adams, Joseph; Herter, Terry; Keller, Luke; Sidher, Sunil; Sinclair, James; Fujiyoshi, Takuya

    2016-04-01

    We present thermal infrared observations of the disk of Uranus at 17-200 μm to deduce its global thermal structure and bulk composition. We combine 17-200 μm filtered photometric measurements by the Herschel PACS and ISO LWS instruments and 19-35 μm filtered photometry and spectroscopy by the SOFIA FORCAST instrument, supplemented by 17-25 μm ground-based photometric filtered imaging of Uranus. Previous analysis of infrared spectroscopic measurements of the disk of Uranus made by the Spitzer IRS instrument yielded a model for the disk-averaged temperature profile and stratospheric composition (Orton et al. 2014a Icarus 243,494; 2014b Icarus 243, 471) that were consistent with submillimeter spectroscopy by the Herschel SPIRE instrument (Swinyard et al. 2014, MNRAS 440, 3658). Our motivation to observe the 17-35 μm spectrum was to place more stringent constraints on the global para-H2 / ortho-H2 ratio in the upper troposphere and lower stratosphere than the ISO SWS results of Fouchet et al. (2003, Icarus 161, 127), who examined H2 quadrupole lines. We will discuss the consistency of these observations with a higher para-H2 fraction than implied by local thermal equilibrium, which would resolve a discrepancy between the Spitzer-based model and observations of HD lines by the Herschel PACS experiment (Feuchtgruber et al. 2013 Astron. & Astrophys. 551, A126). Constraints on the global para-H2 fraction allow for more precise analysis of the far-infrared spectrum, which is sensitive to the He:H2 ratio, a quantity that was not constrained by the Spitzer IRS spectra. The derived model, which assumed the ratio derived by the Voyager-2 IRIS/radio-science occultation experiment (Conrath et al. 1987 J. Geophys. Res. 92, 15003), is inconsistent with 70-200 μm PACS photometry (Mueller et al. 2016 Astron. & Astrophys. submittted) and ISO LWS photometric measurements. However, the model can be made consistent with the observations if the fraction of He relative to H2 were

  18. Ways of Changing the Number and Size Distribution of Ecliptic Comets

    Science.gov (United States)

    Dones, Henry C. Luke; Womack, Maria; Alvarellos, Jose; Bierhaus, Edward B.; Bottke, William; Hamill, Patrick; Nesvorny, David; Robbins, Stuart J.; Zahnle, Kevin

    2017-06-01

    The existence of the Kuiper Belt was proposed because of the need for a low-inclination source for the Jupiter-family comets (JFCs). Indeed, the Kuiper Belt is thought to be the main reservoir of ecliptic comets (ECs), which include the JFCs and Centaurs. Ironically, we still do not know whether the belt, specifically its Scattered Disk, provides an adequate source for the ECs (Volk and Malhotra 2008). ECs are also thought to be the main source of Sun-orbiting impactors on the regular moons of the giant planets (Zahnle et al. 2003 [Z03]). Some models of the cometary orbital distribution used by Z03 and others to estimate impact rates assume comets are indestructible; in fact, many cometssplit, sometimes far from the Sun (Fernández 2009). Assuming shatterproof comets may lead to incorrect results for cometary orbital distributions. Other models impose a physical lifetime for bodies that approach within ~3 AU of the Sun, where sublimation of water ice begins, after which a comet is assumed to be dormant or disrupted (Nesvorný et al. 2017). In reality, some comets (e.g., 29P, Hale-Bopp) are active due to volatiles such as CO and CO2 beyond the orbit of Jupiter (Womack et al. 2017). 174P/Echeclus underwent a 7-magnitude outburst 13 AU from the Sun (Rousselot et al. 2016), and CO emission was recently detected from Echeclus at 6 AU (Wierzchos et al. 2017). We will estimate the effects of several mechanisms on the number and size distribution of comet nuclei as a function of distance from the Sun, including cometary activity and spontaneous disruption; tidal disruption by a giant planet, as happened for Shoemaker-Levy 9; and tidal disruption of binaries, which are numerous among "cold classical" Kuiper Belt Objects (Fraser et al. 2017). We thank the Cassini Data Analysis Program for support.Fernández Y (2009). Planet. Space. Sci. 57, 1218.Fraser WC, et al. (2017). Nat. Astron. 1, 0088.Nesvorný D, et al. (2017). In preparation.Rousselot P, et al. (2016). MNRAS 462, S

  19. Stellar Archaeology and Galaxy Genesis: The Need for Large Area Multi-Object Spectrograph on 8 m-Class Telescopes

    Science.gov (United States)

    Irwin, Mike J.; Lewis, Geraint F.

    The origin and evolution of galaxies like the Milky Way and M31 remain among the key questions in astrophysics. The galaxies we see today in and around the Local Group are representatives of the general field population of the Universe and have been evolving for the majority of cosmic time. As our nearest neighbour systems they can be studied in far more detail than their distant counterparts and hence provide our best hope for understanding star formation and prototypical galaxy evolution over the lifetime of the Universe [K. Freeman, J. Bland-Hawthorn in Annu. Rev. Astron. Astrophys. 40, 487 (2002)]. Significant observational progress has been made, but we are still a long way from understanding galaxy genesis. To unravel this formative epoch, detailed large area multi-object spectroscopy of spatial, kinematic and chemical structures on 8 m-class telescopes are required, to provide the link between local near-field cosmology and predictions from the high-redshift Universe.

  20. "Cosmografia geográfica: a astronomia no ensino de geografia"

    OpenAIRE

    Paulo Henrique Azevedo Sobreira

    2006-01-01

    Esta pesquisa relaciona o Ensino da Astronomia ao Ensino da Geografia e aborda um grande cabedal de temas que expressam relações importantes entre os conhecimentos terrestres e os celestes. Estudou-se um campo que faz parte da Cosmografia e que se constitui em uma releitura na área de Geografia, para o qual se propõe a designação de “Cosmografia Geográfica”, ao invés do nome “Cosmografia”, simplesmente, ou “Geografia Astronômica”. O termo “Cosmografia” está em desuso, e suas atribuições for...

  1. Learning Astronomy by Playing in a Park. (Spanish Title: Aprender AstronoMía Jugando en Una Plaza.) Aprender Astronomia Brincando em Uma Praça

    Science.gov (United States)

    Camino, Néstor

    2012-12-01

    Some public-square games are presented in this paper, considered as didactic modules to help children imagine astronomical processes, based on the concept that learning in Astronomy should be developed to strengthen the relationship of our body with three-dimensional space and time, much in the same way we experience when observing the actual sky, holding a permanent "dialogue" between the actual world and what is to be learned. The games presented (merry-go-rounds and slides) were designed to work on the astronomical concepts related to the translation of the Earth around the Sun, the phases of the Moon and gravity, and on what is perceived by an observer about those phenomena. The description of each game, their physical and astronomical foundations, and a critical comment about their didactical importance are the key parts of the paper. Finally, a recommendation is given about the role teachers should play to be essential partners in the process of learning Astronomy by means of the interaction with these games. Se presentan en este trabajo algunos juegos de plaza, considerados como módulos didácticos para imaginar procesos astronómicos, a partir de la concepción de que el aprendizaje en Astronomía debe desarrollarse fortaleciendo la relación del propio cuerpo con el espacio tridimensional y con el tiempo, tal como se vive al observar el cielo, construyendo un "diálogo" entre el mundo real y los aprendizajes a construir. Los juegos presentados (calesitas y toboganes) fueron diseñados para trabajar sobre la traslación de la Tierra en torno al Sol, las fases de la Luna y la gravedad, y sobre lo que un observador percibe de los mismos. Se da la descripción de cada juego, se discuten sus fundamentos físicos y astronómicos, y se desarrolla una crítica didáctica de los mismos. Finalmente, se comenta el rol que deberían tener los docentes en el acompañamiento a los aprendices en el proceso de interacción con los juegos presentados. Apresentam-se neste

  2. Proyecto para la medición sistemática de seeing en CASLEO

    Science.gov (United States)

    Fernández Lajus, E.; Forte, J. C.

    La calidad del seeing astronómico es ciertamente uno de los parámetros mas importantes que caracterizan el sitio de un observatorio. Por tanto se desea determinar si el alto valor de seeing observado con el telescopio de 2.15 m se debe a efectos internos y/o del entorno a la cupula o si se debe simplemente al seeing propio del lugar. El actual mecanismo de refrigeración del espejo primario del 2.15, parece haber mejorado notablemente la calidad del seeing. Sin embargo se hace necesario saber hasta que punto el valor del seeing puede ser mejorado. La primera etapa del proyecto consistió en la puesta a punto del telescopio emplazado para este propósito y la adquisición de las primeras medidas tentativas de seeing.

  3. Spectrophotometric intracutaneous analysis for differential diagnosis of pigmented skin lesions

    Directory of Open Access Journals (Sweden)

    Е. V. Filonenko

    2013-01-01

    Full Text Available The non-invasive diagnosis of pigmented skin lesions by spectrophotometric intracutaneous analysis (SIA-scopy using device for dermatoscopy (SIAscope V by Astron Clinica, Ltd was approved in P.A.Herzen Moscow Cancer Research Institute. The method is based on analysis of light interaction with wavelength of 440–960 nm anf human skin, which is recorded by change of image on scan. The comparative analysis of SIA-scopy and histological data in 327 pigmented skin lesions in 147 patients showed, that SIA had high diagnostic efficiency for cutaneous melanoma: the sensitivity was 96%, specifity – 94%, diagnostic accuracy – 94%. For study of malignant potential of pigmented lesions by SIA-scopy the most informative capacity was obtained for assessment of melanin in papillary dermis, status of blood vessels and collagen fibres (SIA-scans 3, 4, 5.

  4. Time Resolved Precision Differential Photometry with OAFA's Double Astrograph

    Science.gov (United States)

    González, E. P. A.; Podestá, F.; Podestá, R.; Pacheco, A. M.

    2018-01-01

    For the last 50 years, the Double Astrograph located at the Carlos U. Cesco station of the Observatorio Astronómico Félix Aguilar (OAFA), San Juan province, Argentina, was used for astrometric observations and research. The main programs involved the study of asteroid positions and proper motions of stars in the Southern hemisphere, being the latter a long time project that is near completion from which the SPM4 catalog is the most recent version (Girard et al. 2011). In this paper, new scientific applications in the field of photometry that can be accomplished with this telescope are presented. These first attempts show the potential of the instrument for such tasks.

  5. Repaso del Sabio Caldas

    Directory of Open Access Journals (Sweden)

    Jaime Paredes Pardo

    1983-01-01

    Full Text Available En Popayán aún se conserva la casa donde nació el sabio Francisco José de Caldas. Está situada en la esquina de la carrera 5a. con la calle 3a., en pleno barrio de la Pamba. Es una construcción robusta de líneas austeras y como especialidad única cuenta con un patio en cuyo centro se levanta un observatorio astronómico, obra del propio Caldas cuando estaba joven. Varios instrumentos que le fueron útiles fabricó para el observatorio, desde donde podía seguir el giro de los astros. Antes cuando era apenas un niño, su madre tenía que reprenderlo con alguna frecuencia porque tardaba demasiado en el estudio de los libros.

  6. A photometric survey of Near-Earth Objects in support of the NEOShield-2 project

    Science.gov (United States)

    Ieva, S.; Dotto, E.; Mazzotta Epifani, E.; Perna, D.; Barucci, M. A.; Di Paola, A.; Micheli, M.; Perozzi, E.; Speziali, R.; Lazzarin, M.; Bertini, I.; Giunta, A.; Lazzaro, D.; Arcoverde, P.

    2017-09-01

    More than 85% of the 16,000 NEOs discovered up to now lack a physical characterization. The study of their physical properties is essential to define a proper mitigation scenario. One of the main aims of the NEOShield-2 project (2015-2017), financed by the European Community in the framework of the Horizon 2020 program, is therefore to retrieve physical properties of a wide number of NEOs, in order to design impact mitigation missions and assess the consequences of an impact on Earth. We present the results obtained during a 2-year Long-Term Program at the Telescopio Nazionale Galileo (TNG, La Palma, Spain), where we carried out BVRI photometry of about 150 NEOs, and the analysis of the phase curves obtained at the Campo Imperatore telescope (L'Aquila, Italy) and the Observatório Astronômico do Sertão de Itaparica (Nova Itacuruba, Brazil).

  7. Alfabetización en Astronomía de docentes de Educación Primaria y de Educación Secundaria en La Plata

    Science.gov (United States)

    De Biasi, M. S.; Orellana, R. B.

    2014-10-01

    La educación de este siglo tiene como uno de sus retos alcanzar la alfabetización cientfica de todos los ciudadanos para que comprendan y tomen decisiones sobre el mundo natural y sus cambios originados por la actividad humana utilizando el conocimiento científico. En esta misión los docentes de los niveles obligatorios de enseñanza juegan un papel clave por su rol de agentes multiplicadores del conocimiento. Se requiere, entonces de una adecuada alfabetización en ciencias de los docentes o, como mínimo, que dominen los temas científicos a enseñar. En el campo de la Astronomía, numerosas investigaciones han señalado que maestros de primaria y estudiantes de profesorados poseen una escasa formación en estos temas (Camino 1995 y 1999, Gangui 2010), que frecuentemente presentan a los alumnos concepciones alternativas o no científicas de los fenómenos astronómicos cotidianos (Kriner 2004, Vega Navarro 2007, Gangui et al 2010); a lo que se suma la presentación confusa o errónea de algunos temas astronómicos en los textos escolares (Kriner 2004). Desde 2011, la Facultad de Ciencias Astronómicas y Geofísicas, UNLP, ofrece un curso de capacitación destinado a fortalecer y actualizar los contenidos académicos y didácticos de los docentes del distrito La Plata utilizando diversas estrategias didácticas. Los contenidos comprenden los temas astronómicos de los diseños curriculares vigentes. La evaluación diagnóstica de los conocimientos previos de los docentes cursantes sobre los contenidos de mayor presencia en los diseños curriculares mostró resultados similares a las investigaciones arriba mencionadas. Referente a los movimientos de la Tierra, en promedio, el 54% poseía conceptos erróneos y el 16% no los sabía; con referencia a la Luna el 56% poseía conceptos erróneos y un 4% no los sabía. Los resultados del curso mostraron que el 95% de los docentes revirtió sus conceptos previos erróneos, que adquirió criterios para la búsqueda de

  8. En memoria de un científico mexicano: Francisco Díaz Covarrubias

    OpenAIRE

    Hermosillo-Villalobos, Juan J.

    1989-01-01

    Texto en torno al ingeniero y científico mexicano Francisco Díaz Covarrubias en conmemoración al centenario de su deceso. Covarrubias cursó la carrera de ingeniero topógrafo en el Colegio de Minería en la Ciudad de México, recibiendo los máximos horones en 1853. Algunas de sus principales aportaciones fueron el levantamiento de un Atlas del Valle de México, la fundación y su trabajo como director del Observatorio Astronómico Nacional, y la realización de la expedición a Japón en diciembre de ...

  9. Cosmology and the Subgroups of Gamma-ray Bursts

    Directory of Open Access Journals (Sweden)

    A. Mészáros

    2011-01-01

    Full Text Available Both short and intermediate gamma-ray bursts are distributed anisotropically in the sky (Mészáros, A. et al. ApJ, 539, 98 (2000, Vavrek, R. et al. MNRAS, 391, 1 741 (2008. Hence, in the redshift range, where these bursts take place, the cosmological principle is in doubt. It has already been noted that short bursts should be mainly at redshifts smaller than one (Mészáros, A. et al. Gamma-ray burst: Sixth Huntsville Symp., AIP, Vol. 1 133, 483 (2009; Mészáros, A. et al. Baltic Astron., 18, 293 (2009. Here we show that intermediate bursts should be at redshifts up to three.

  10. Russian Virtual Observatory: data sources

    Science.gov (United States)

    Malkov, O.; Dluzhnevskaya, O.; Bakanas, E.; Kilpio, E.; Kniazev, A.; Kovaleva, D.; Mironov, A.; Pakhomov, Yu.; Ryabchikova, T.; Rykhlova, L.; Sachkov, M.; Sazonov, S.; Zhukov, A.

    The purpose of this review is to analyze main directions of creation and functioning of major data sources developed by Russian astronomers or with their participation and to compare them with the worldwide trends in these fields. We discuss astronomical space missions of the past, present, and future (Astron, INTEGRAL, WSO-UV, Spectrum Roentgen Gamma, Lyra-B), high-quality photometric atlases and catalogues, and spectroscopic data sources, primarily VALD and the global VAMDC framework for the maintenance and distribution of atomic and molecular data. We describe collection, analysis, and dissemination of astronomical data on minor bodies of the Solar System and on variable stars. Also described is the project joining data for all observational types of binary and multiple stars, Binary star DataBase (BDB).

  11. New International Agreements About Space Techniques Among Argentina, China and France

    Science.gov (United States)

    Pacheco, A. M.; Podestá, R.; Actis, E.; Adarvez, S.; Quinteros, J.; Li, J.; Saunier, J.; Podestá, F.; Ramos, F.; Aguilera, J.; Sosa, G.; Hauser, D.

    2018-01-01

    The International Earth Rotation and Reference Systems (IERS) is in charge of defining and materializing celestial reference systems (ICRS - ICRF) and terrestrial reference systems (ITRS - ITRF). In order to perform this task it uses data from the following techniques: Very Long Baseline Interferometry (VLBI), Satellite Laser Ranging (SLR), Global Navigation Satellite System (GNSS) and Doppler Orbitography and Radiopositioning Integrated by Satellite (DORIS). Nowadays, the Observatorio Astronómico Félix Aguilar (OAFA) has two instruments with these advanced techniques: SLR and a permanent GNSS station. In the nearby future a 40 m diameter radio telescope will be available that will be operated in VLBI mode along with a DORIS buoy which will be co-localized with a SLR telescope and GNSS antennas. In this way OAFA will become a zero station, first class, of the ITRF 2014 frame.

  12. Probabilities for Solar Siblings

    Science.gov (United States)

    Valtonen, Mauri; Bajkova, A. T.; Bobylev, V. V.; Mylläri, A.

    2015-02-01

    We have shown previously (Bobylev et al. Astron Lett 37:550-562, 2011) that some of the stars in the solar neighborhood today may have originated in the same star cluster as the Sun, and could thus be called Solar Siblings. In this work we investigate the sensitivity of this result to galactic models and to parameters of these models, and also extend the sample of orbits. There are a number of good candidates for the sibling category, but due to the long period of orbit evolution since the break-up of the birth cluster of the Sun, one can only attach probabilities of membership. We find that up to 10 % (but more likely around 1 %) of the members of the Sun's birth cluster could be still found within 100 pc from the Sun today.

  13. Errores sistemáticos del Catálogo Fundamental FK5, deducidos de las observaciones con Astrolabio Fotoeléctrico PAII, en el Hemisferio Sur

    Science.gov (United States)

    Manrique, W. T.; Podestá, R. C.; Alonso, E.; Actis, E. V.; Pacheco, A. M.; Bustos, G.; Lizhi, L.; Zezhi, W.; Fanmiao, Z.; Hongqi, W.; Perdomo, R.; González, A.; Gómez, G.

    Se dan los resultados obtenidos de los Errores Sistemáticos del Catálogo Fundamental FK5, Δ α δ, Δ α α, Δ δ α y Δ δ δ, derivados de las observaciones estelares con el Astrolabio Fotoeléctrico PAII del Observatorio de Beijing instalado en el Observatorio Astronómico ``Félix Aguilar'' de San Juan, de acuerdo al Proyecto de Colaboración entre los observatorios de San Juan, Beijing y La Plata. Se han usado los residuos seleccionados de 11000 estrellas aproximadamente, derivados de más de 400000 pasajes estelares en 1550 días, desde Febrero de 1992 a Marzo de 1997. La precisión media de los residuos es de 0,"043.

  14. THE BREAKDOWN OF CLASSICAL GRAVITY?

    OpenAIRE

    M. A. Jiménez; X. Hernández,; C. Allen

    2014-01-01

    Bajo el supuesto de que la ley de la gravedad de Newton y la Relatividad General (RG) son v ́alidas a todas las escalas, surge la hip ́otesis de la existencia de materia oscura para poder explicar l a din ́amica de los sistemas astron ́omicos a escalas gal ́acticas y extragal ́acticas. Otra posibili dad, que no involucra la existencia de ning ́un componente ex ́otico, es modificar la ley de la gravedad a escalas donde la aceleraci ́on es menor que a 0 = 1 . 2 × 10 − 8 cm s − 2 . Las ́orbitas ...

  15. Supernovas, faros en el universo: medición de la distancia a ASASSN-15hx

    Directory of Open Access Journals (Sweden)

    Ramona Núñez López

    2016-12-01

    Full Text Available Difícil pensar en un evento astronómico tan relevante y polifacético como la gigantesca explosión de supernova, que en breves segundos destruye su estrella, creando un gran número de elementos pesados. El inmenso brillo de las supernovas permite observarlas a enormes distancias, para así obtener información cosmológica. En este trabajo abordamos en general el tema de supernovas, enfocándonos luego al estudio de la supernova de tipo Ia ASASSN-15hx. Presentamos las observaciones realizadas en diferentes filtros y mostramos un método basado en el ancho de su curva de luz para estimar su distancia y corrimiento al rojo. Los valores obtenidos coinciden con información encontrada en la literatura y las incertidumbres obtenidas están dentro del rango de las encontradas con otros métodos.

  16. Los hebreos: Un legado religioso

    Directory of Open Access Journals (Sweden)

    Ligia Carvajal Mena

    2014-11-01

    Full Text Available Los primeros asentamientos humanos tuvieron lugar en las riberas de ríos como el Éufrates, Tigris y Nilo. Estas tierras, por su fertilidad, se convirtieron en cuna de culturas que dejaron un legado importante para el desarrollo de la humanidad. En el marco de esas culturas destaca la hebrea que asume aspectos culturales foráneos, los recompone y da un salto original en su cultura, especialmente en el ámbito religioso. Lo anterior al establecer inequívocamente el monoteísmo, realizar mejores construcciones (entre lo religioso y lo astronómico y crear un Dios con fuerte contenido ético, que trasciende del ámbito nacional al universal.

  17. Concepciones alternativas sobre Astronomía de profesorado español en formación

    Directory of Open Access Journals (Sweden)

    María-Mercedes Varela-Losada

    2015-12-01

    Full Text Available ResumenEl proceso de enseñanza y aprendizaje de la Astronomía parece entrañar importantes dificultades, particularmente propiciando la generación de concepciones alternativas, como han mostrado numerosas investigaciones procedentes de diferentes contextos. El objetivo de este estudio es indagar sobre concepciones alternativas de profesorado en formación relacionadas con aspectos astronómicos, investigando si en el marco español aparecen los mismos esquemas alternativos que en otros contextos. Los resultados ponen en evidencia que el alumnado mencionado posee un gran número de concepciones alternativas sobre astronomía básica y que estas son similares a las encontradas en otros países.

  18. A family of stacked central configurations in the planar five-body problem

    Science.gov (United States)

    Cornelio, J. Lino; Álvarez-Ramírez, M.; Cors, Josep M.

    2017-11-01

    We study planar central configurations of the five-body problem where three bodies, m_1, m_2 and m_3, are collinear and ordered from left to right, while the other two, m_4 and m_5, are placed symmetrically with respect to the line containing the three collinear bodies. We prove that when the collinear bodies form an Euler central configuration of the three-body problem with m_1=m_3, there exists a new family, missed by Gidea and Llibre (Celest Mech Dyn Astron 106:89-107, 2010), of stacked five-body central configuration where the segments m_4m_5 and m_1m_3 do not intersect.

  19. La gravedad en Bruno, Kleper y Newton. la distribución de la materia y sus implicaciones cosmológicas

    Directory of Open Access Journals (Sweden)

    M. Diego Pintado

    2016-10-01

    Full Text Available En este trabajo se describe en modo sucinto el papel fundamental y determinante del problema de la gravitación universal en la historia de la cosmología moderna, indagándose así mismo los factores que le dieron origen, principalmente la proposición de la formulación de la ley de gravedad, sus antecedentes, y a su vez se repasan los problemas astrofísicos, astronómicos y filosóficos de este nuevo esquema cosmológico. El esquema de esta monografía traza un breve examen epistemológico, luego un repaso por el origen y gestación del concepto de gravitación universal, y finalmente un análisis del desarrollo de la cosmología moderna, o newtoniana, entorno a los problemas implicados por la ley de gravedad.

  20. Comportamiento de la cromósfera solar en la línea H-alpha durante el ciclo 23

    Science.gov (United States)

    Davoli, D.; Aquilano, R.; Missio, H.

    Using the instrumental of the Observatorio Astronómico Municipal de Rosario (OAMR), we analyze the solar chromospheric activity during an approximate period of 11 years. The instrument is a Carl Zeiss refractor telescope of 150 mm aperture and 2250 mm of focal distance with monochromatic filter in the H-alpha line. We take as proxy for the solar activity the area covered by chromospheric plages. Simultaneously, we determine the relative wolf number from observations of the solar photosphere. We describe our technique and the results obtained. We observe 2 maxima of solar activity in the years 2000 and 2001 respectively, and a later decrease of this activity with low average values starting around 2006 that corresponds to the end of cycle 23. FULL TEXT IN SPANISH

  1. Approximate analytical time-domain Green's functions for the Caputo fractional wave equation.

    Science.gov (United States)

    Kelly, James F; McGough, Robert J

    2016-08-01

    The Caputo fractional wave equation [Geophys. J. R. Astron. Soc. 13, 529-539 (1967)] models power-law attenuation and dispersion for both viscoelastic and ultrasound wave propagation. The Caputo model can be derived from an underlying fractional constitutive equation and is causal. In this study, an approximate analytical time-domain Green's function is derived for the Caputo equation in three dimensions (3D) for power law exponents greater than one. The Green's function consists of a shifted and scaled maximally skewed stable distribution multiplied by a spherical spreading factor 1/(4πR). The approximate one dimensional (1D) and two dimensional (2D) Green's functions are also computed in terms of stable distributions. Finally, this Green's function is decomposed into a loss component and a diffraction component, revealing that the Caputo wave equation may be approximated by a coupled lossless wave equation and a fractional diffusion equation.

  2. Continuity of the robustness of contextuality of empirical models

    Science.gov (United States)

    Meng, HuiXian; Cao, HuaiXin; Wang, WenHua; Chen, Liang; Fan, Yajing

    2016-10-01

    Recently, the robustness of contextuality (RoC) of an empirical model was discussed in [Sci. China-Phys. Mech. Astron. 59, 640303 (2016)], many important properties of the RoC have been proved except for its boundedness and continuity. The aim of this paper is to find an upper bound for the RoC over all of empirical models and prove that the RoC is a continuous function on the set of all empirical models. Lastly, a relationship between the RoC and the extent of violating the noncontextual inequalities is established for an n-cycle contextual box. This relationship implies that the RoC can be used to quantify the contextuality of n-cycle boxes.

  3. Application of Three-Dimensional Models for the Teaching of Time Zones. (Breton Title: Aplicação de Modelos Tridimensionais Para o Ensino de Fusos Horários.) Aplicación de Modelos Tridimensionales Para la Enseñanza de Husos Horarios

    Science.gov (United States)

    Azevedo Sobreira, Paulo Henrique

    2012-07-01

    There are several interesting astronomical topics that must be addressed in the High School and Elementary/Middle School in the disciplines of Geography and of Sciences. Among them, the topic of time zones which is one of the most important to understand the correlation of the Earth's rotation and its implications on daily activities of citizens in local scale, regional and global scales which involve problems of time differences. For the teaching of time zones in the lessons of Geography, for example, there are bi-dimensional representations of thematic maps of world time zones, textbooks and atlas. It happens that teachers face some difficulties to permit its students to view three-dimensionally this astronomical phenomenon from the textbooks available in schools. The aim of this paper is to present two proposals with low-cost materials, which allow the preparation of three-dimensional models for the teaching of time zones. Há vários temas astronômicos interessantes que devem ser trabalhados nos Ensinos Médio e Fundamental, nas disciplinas de Geografia e de Ciências. Entre eles, o tema dos fusos horários que é um dos mais importantes para se correlacionar a rotação da Terra e suas implicações nas atividades cotidianas dos cidadãos em escala local, regional e global, que envolvem problemas de diferenças horárias. Para o ensino dos fusos horários nas aulas de Geografia, por exemplo, há representações bidimensionais de mapas temáticos de fusos horários mundiais, nos livros didáticos e nos atlas. Ocorre que os professores enfrentam algumas dificuldades para possibilitar aos seus alunos a visão tridimensional deste fenômeno astronômico, a partir dos materiais didáticos disponíveis nas escolas. O objetivo deste trabalho é apresentar duas propostas para a confecção de materiais de baixo custo, que possibilitem a elaboração de modelos tridimensionais para o ensino dos fusos horários. Hay algunos temas astronómicos interesantes que se

  4. Theory and Simulations of Refractive Substructure in Resolved Scatter-broadened Images

    Science.gov (United States)

    Johnson, Michael D.; Gwinn, Carl R.

    2015-06-01

    At radio wavelengths, scattering in the interstellar medium distorts the appearance of astronomical sources. Averaged over a scattering ensemble, the result is a blurred image of the source. However, Narayan & Goodman and Goodman & Narayan showed that for an incomplete average, scattering introduces refractive substructure in the image of a point source that is both persistent and wideband. We show that this substructure is quenched but not smoothed by an extended source. As a result, when the scatter-broadening is comparable to or exceeds the unscattered source size, the scattering can introduce spurious compact features into images. In addition, we derive efficient strategies to numerically compute realistic scattered images, and we present characteristic examples from simulations. Our results show that refractive substructure is an important consideration for ongoing missions at the highest angular resolutions, and we discuss specific implications for RadioAstron and the Event Horizon Telescope.

  5. Increase of the mean Sun-Earth distance caused by a secular mass accumulation

    Science.gov (United States)

    Wilhelm, Klaus; Dwivedi, Bhola N.

    2013-09-01

    Based on many planetary observations between the years 1971 and 2003, Krasinsky and Brumberg (Celest. Mech. Dyn. Astron. 90:267-288, 2004) have estimated a rate of increase in the mean Sun-Earth distance of (15±4) m per century. Together with other anomalous observations in the solar system, this increase appears to be unexplained (Lämmerzahl et al. in Astrophys. Space Sci. Lib., vol. 349, pp. 75-101, 2008). We explain these findings by invoking a recently proposed gravitational impact model (Wilhelm et al. in Astrophys. Space Sci. 343:135-144, 2013) that implies a secular mass increase of all massive bodies. This allows us to formulate a quantitative understanding of the effect within the parameter range of the model with a mass accumulation rate of the Sun of (6.4±1.7)×1010 kg s-1.

  6. Numerical integration of relativistic equations of motion for Earth satellites

    Science.gov (United States)

    San Miguel, A.

    2009-01-01

    The equations of motion proposed by Brumberg for an artificial satellite around the Earth (Celest Mech Dyn Astron 88:209, 2004), in which the relativistic effects due to the Earth’s oblatness and the gravitational action caused by a third body are added to those perturbations considered in the International Earth Rotation and Reference System Service (2003) convention, are here integrated numerically. To compute the solution of the time-dependent Langrangian system for a gravitational satellite Earth Sun model we consider a six-order partitioned Runge Kutta integrator, whose coefficients satisfy the condition of symplecticity. A comparison with the classical Adams Basforth Moulton method allows to verify the good-performance of the partitioned Runge Kutta method both in the description of the evolution of the satellite energy and in the efficiency of the method when applied to a long-term integration.

  7. A search for transit timing variations and orbital decay in WASP-46b

    Science.gov (United States)

    Petrucci, R.; Jofré, E.; Ferrero, L. V.; Cúneo, V.; Saker, L.; Lovos, F.; Gómez, M.; Mauas, P.

    2018-02-01

    We present 12 new transit observations of the exoplanet WASP-46b obtained with the 1.54-m telescope at Estación Astrofísica de Bosque Alegre (EABA, Argentina) and the 0.40-m Horacio Ghielmetti and 2.15-m Jorge Sahade telescopes at Complejo Astronómico El Leoncito (CASLEO, Argentina). We analyse them together with 37 light curves from the literature to re-determine the physical parameters and search for additional planets via transit timing variations (TTVs). We consider the 31 transits with uncertainties in their mid-transit times (e_T0) 7 × 103 on the tidal quality factor and determine that an additional 6 yr baseline is required to rule out Q⋆ < 105.

  8. Numerical Simulations of Solar Spicule Jets at a Magnetic Null-Point

    Science.gov (United States)

    Smirnova, V.; Konkol, P. M.; Solov'ev, A. A.; Murawski, K.

    2016-11-01

    Two-dimensional numerical simulations of jet-like structures in the solar atmosphere are performed. These structures result from a pressure pulse that is launched at the null point of a potential magnetic arcade. The plasma jet exhibits a double structure with two components: (a) dense, cool, and short vertical stream and (b) a less dense, hot and tall part of the jet. The upper part of the hot and tall jet may represent a direct response of the system to the pressure pulse launched at the null point, and the second, slower cool and dense part of the jet is formed later through the stretching up of the stream as a result of plasma evacuation from the top of the magnetic arcade. Numerical results show that jet-like structures mimic some properties of both type I and type II spicules, according to the classification provided by De Pontieu et al. ( Publ. Astron. Soc. Japan 59, S655, 2007).

  9. “Propuesta didáctica para pasar de preconceptos comunes a conceptos científicos con estudiantes de quinto grado de primaria a partir del desarrollo histórico del Zodíaco hasta llegar a la Eclíptica”

    OpenAIRE

    Jiménez Jiménez, Alexandra

    2011-01-01

    Se presenta el análisis y las respuestas encontradas en un instrumento de indagación en el que se da cuenta de las ideas previas que tienen los niños del grado quinto de la básica primaria de la Institución Educativa Departamental Antonio Nariño del municipio de Cajicá, al rededor de los conceptos astronómicos relacionados con el Zodíaco y la Eclíptica y se presentan los resultados parciales de la propuesta didáctica que se elaboró, en respuesta a dicha indagación. Esta propuesta fue es...

  10. Alternative approaches to plasma confinement

    Science.gov (United States)

    Roth, J. R.

    1978-01-01

    The paper discusses 20 plasma confinement schemes each representing an alternative to the tokamak fusion reactor. Attention is given to: (1) tokamak-like devices (TORMAC, Topolotron, and the Extrap concept), (2) stellarator-like devices (Torsatron and twisted-coil stellarators), (3) mirror machines (Astron and reversed-field devices, the 2XII B experiment, laser-heated solenoids, the LITE experiment, the Kaktus-Surmac concept), (4) bumpy tori (hot electron bumpy torus, toroidal minimum-B configurations), (5) electrostatically assisted confinement (electrostatically stuffed cusps and mirrors, electrostatically assisted toroidal confinement), (6) the Migma concept, and (7) wall-confined plasmas. The plasma parameters of the devices are presented and the advantages and disadvantages of each are listed.

  11. International data transfer for space very long baseline interferometry

    Science.gov (United States)

    Wiercigroch, Alexandria B.

    1994-01-01

    Space very long baseline interferometry (SVLBI) experiments using a TDRSS satellite have successfully demonstrated the capability of using spacecraft to extend the effective baseline length of VLBI observations beyond the diameter of the Earth, thereby improving the resolution for imaging of active galactic nuclei at centimeter wavelengths. As a result, two spacecraft dedicated to SVLBI, VSOP (Japan) and RadioAstron (Russia), are scheduled to be launched into high Earth orbit in 1996 and 1997. The success of these missions depends on the cooperation of the international community in providing support from ground tracking stations, ground radio telescopes, and correlation facilities. The timely exchange and monitoring of data among the participants requires a well-designed and automated international data transfer system. In this paper, we will discuss the design requirements, data types and flows, and the operational responsibilities associated with the SVLBI data transfer system.

  12. RADIOASTRON OBSERVATIONS OF THE QUASAR 3C273: A CHALLENGE TO THE BRIGHTNESS TEMPERATURE LIMIT

    Energy Technology Data Exchange (ETDEWEB)

    Kovalev, Y. Y.; Kardashev, N. S.; Voitsik, P. A.; Kovalev, Yu. A.; Lisakov, M. M.; Sokolovsky, K. V. [Astro Space Center of Lebedev Physical Institute, Profsoyuznaya 84/32, 117997 Moscow (Russian Federation); Kellermann, K. I. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475 (United States); Lobanov, A. P.; Zensus, J. A.; Anderson, J. M.; Bach, U.; Kraus, A. [Max-Planck-Institute for Radio Astronomy, Auf dem Hügel 69, D-53121 (Germany); Johnson, M. D. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Gurvits, L. I. [Joint Institute for VLBI ERIC, P.O. Box 2, 7990 AA Dwingeloo (Netherlands); Jauncey, D. L. [CSIRO Astronomy and Space Sciences, Epping, NSW 1710 (Australia); Ghigo, F. [National Radio Astronomy Observatory, Rt. 28/92, Green Bank, WV 24944-0002 (United States); Ghosh, T.; Salter, C. J. [Arecibo Observatory, NAIC, HC3 Box 53995, Arecibo, Puerto Rico, PR 00612 (United States); Petrov, L. Yu. [Astrogeo Center, 7312 Sportsman Drive, Falls Church, VA 22043 (United States); Romney, J. D. [National Radio Astronomy Observatory, P.O. Box O, 1003 Lopezville Road, Socorro, NM 87801-0387 (United States)

    2016-03-20

    Inverse Compton cooling limits the brightness temperature of the radiating plasma to a maximum of 10{sup 11.5} K. Relativistic boosting can increase its observed value, but apparent brightness temperatures much in excess of 10{sup 13} K are inaccessible using ground-based very long baseline interferometry (VLBI) at any wavelength. We present observations of the quasar 3C 273, made with the space VLBI mission RadioAstron on baselines up to 171,000 km, which directly reveal the presence of angular structure as small as 26 μas (2.7 light months) and brightness temperature in excess of 10{sup 13} K. These measurements challenge our understanding of the non-thermal continuum emission in the vicinity of supermassive black holes and require a much higher Doppler factor than what is determined from jet apparent kinematics.

  13. La Enseñanza/Aprendizaje del Modelo Sol-Tierra Análisis de la Situación Actual y Propuesta de Mejora Para la Formación de los Futuros Profesores de Primaria

    Science.gov (United States)

    Martínez Sebastià, Bernat

    2004-12-01

    This work is an extened summary of the autor's PhD thesis. It deals with the teaching of astronomy (day/night, seasons) in primary school. At first, students teachers' undestanding of astronomical concepts related to Sun-Earth system have been analysed. Taking into account the results of the previous analysis and using a socio-constructivist approach a teaching sequence has been designed. This sequence has been tested with different groups of students teachers showing an improvement in their undestanding of elementary astronomical concepts. El trabajo que presentamos es un resumen extenso de la tesis doctoral del autor. El enfoque utilizado ha sido tratar de ligar la investigación sobre las ideas, razonamientos y obstáculos de los profesores de primaria con la planificación de la enseñanza del modelo Sol-Tierra que permite explicar el ciclo día/noche y las estaciones. En primer lugar, se ha procedido a realizar un análisis crítico de los resultados que se obtienen en el aprendizaje de los contenidos astronómicos en la enseñanza habitual. En segundo lugar se ha diseñado un curriculum potencialmente superador de esta situación desde una orientación que concibe la enseñanza y el aprendizaje como un proceso de construcción de conocimientos en una estructura problematizada. Finalmente, esta secuencia didáctica ha sido experimentada con diferentes grupos de estudiantes de magisterio, mostrando una mejora relevante en la comprensión de los conceptos astronómicos fundamentales.

  14. Projeto observatórios virtuais: educação através de telescópios robóticos

    Science.gov (United States)

    Santana, P. H. S.; Shida, R. Y.

    2003-08-01

    O principal objetivo do projeto Observatórios Virtuais é o ensino na área de ciências através de atividades práticas desenvolvidas em colaboração entre instituições de pesquisa em astronomia e escolas de ensino médio e fundamental. Este ano deverá ser concluída a implantação do programa piloto de estudos, pesquisas e observação astronômica direta, com utilização em tempo real de telescópios robóticos, que assim funcionarão como "observatórios virtuais". O objetivo pedagógico das atividades práticas baseadas nas imagens atronômicas é desenvolver as habilidades e competências dos alunos no uso do método científico. Para isso, serão realizados projetos interdisciplinares, a partir de observações astronômicas, já que a astronomia é uma área interdisciplinar por excelência. Essas atividades terão níveis diferenciados de complexidade, que podem ser adequados aos vários graus do ensino e realidades regionais. Será dada ênfase ao desenvolvimento e aplicação em São Paulo, onde atua a equipe do IAG/USP. Como resultados apresentados no presente trabalho, temos a criação de um software em português para o processamento de imagens obtidas através de CCDs e a elaboração de material para as atividades educacionais relacionadas.

  15. Millimeter and Submillimeter Observations of Comet 67P's Nucleus, Gas, and Dust with the Rosetta/MIRO Instrument

    Science.gov (United States)

    Hofstadter, Mark

    2016-04-01

    The Microwave Instrument for the Rosetta Orbiter (MIRO) has been making measurements of comet 67P/C-G since June 2014, when the comet was 3.92 AU from the Sun and Rosetta was approximately 400,000 km from the nucleus. Those first observations were spatially unresolved measurements of the 556 GHz water line, used to infer the abundance and velocity of water vapor in the coma (Gulkis et al. 2015, Science 347). In the almost two years since that time, as the spacecraft has moved closer to the nucleus and the comet has become more active (perihelion at 1.2 AU from the Sun occurred in August 2015), MIRO's submillimeter spectrometer (working at frequencies near 550 GHz, or wavelengths near 0.5 mm) has been used to determine the velocity, abundance, and spatial distribution of H216O, H217O, H218O, CH3OH, NH3, and CO in the coma as a function of time (e.g. water is discussed by Biver et al. 2015 and Lee et al. 2015, Astron. and Astrophys. 583). In addition to its submillimeter spectrometer, MIRO has two broad band continuum channels operating at wavelengths near 0.5 and 1.6 millimeter. These channels are designed to probe the nucleus ˜1 millimeter to 10 cm below the surface. Data have been used to infer properties such as thermal inertia, porosity, and ice content as functions of location, depth, and time (e.g. Schloerb et al. 2015 and Choukroun et al. 2015, Astron. and Astrophys. 583). These channels have also been used to map the distribution of relatively large dust grains (radius > ˜1 mm) in the inner coma of the comet, with the potential to constrain models of dust acceleration, cooling, and fragmentation. This talk will review the latest results from MIRO's measurements of the nucleus, coma, and dust, and discuss some of the processes that couple these components of the comet.

  16. The Universe Observing Center a modern center to teach and communicate astronomy

    Science.gov (United States)

    Ribas, Salvador J.

    2011-06-01

    The Universe Observing Center is one of the parts of the Parc Astronòmic Montsec (PAM). PAM is an initiative of the Catalan government, through the Consorci del Montsec (Montsec Consortium), to take advantage of the capabilities and potential of the Montsec region to develop scientific research, training and outreach activities, particularly in the field of Astronomy. The choice of the Montsec mountains to install the PAM was motivated by the magnificent conditions for observing the sky at night; the sky above Montsec is the best (natural sky free of light pollution) in Catalonia for astronomical observations. The PAM has two main parts: the Observatori Astronòmic del Montsec (OAdM) and the Universe Observing Center (COU). The OAdM is a professional observatory with an 80-cm catadioptric telescope (Joan Oró Telescope). This telescope is a robotic telescope that can be controlled from anywhere in the world via the Internet. The COU is a large multipurpose center which is intended to become an educational benchmark for teaching and communicate astronomy and other sciences in Catalonia. The management of the COU has three main goals: 1) Teach primary and secondary school students in our Educational Training Camp. 2) Teach university students housing the practical astronomy lectures of the universities. 3) Communicate astronomy to the general public. The COU comprises special areas for these purposes: the Telescopes Park with more than 20 telescopes, a coelostat for solar observations and two dome containing full-automated telescopes. The most special equipment is ``The Eye of Montsec'', with its 12m dome containing a multimedia digital planetarium and a platform for direct observation of the sky and the environment. During 2009 we expect around 10000 visitors in Montsec area to enjoy science with Montsec dark skies and an special natural environment.

  17. Calidad de Imagen del Telescopio UNAM212

    Science.gov (United States)

    Cobos, F. J.; Teiada de Vargas, C.

    1987-05-01

    El telescopio UNAM2l2, del Observatorio Astronómico Nacional, situado en la Sierra de San Pedro Mártir (Baja California, México), cumplira en un futuro muy cercano siete años de uso para fines de investigación astronómica. Aunque en este tiempo no se ha efectuado un estudio sistemático acerca de su comportamiento óptico y de los factores que influyen en la calidad de las imágenes, se han realizado pruebas diversas, estudios parciales y reuniones especificas, cuyos resultados no siempre se han difundido ampliamente y generalmente no se han presentado por escrito. Es por ello que hemos creido necesario intentar una recopilación de la información existente para poder con ella establecer un diagnóstjco que, aunque no sea definitivo, sirva de base para futuros trabajos tendientes a optimizar el comportamiento óptico del telescopio. Es evidente que un buen número de las conclusiones que se presentan son resultado del trabajo de muchas personas ó de esfuerzos colectivos. Asimismo, hemos tratado de localizar información bibliográfica que pueda ser de utilidad. Nuestro objetivo primordial ha consistido en centrarnos en la óptica del telescopio y su calidad, pero también se han considerado otros aspectos que puedan afectar las imágenes obtenidas tales como: celda del primario, `seeing' local y externo, flexiones posibles en la estructura mecánica del telescopio, etc.

  18. Polarimetry of M-type asteroids

    Science.gov (United States)

    Gil-Hutton, R.

    2007-03-01

    Aims:Results of a polarimetric program at Complejo Astronómico El Leoncito (Casleo), San Juan, Argentina are presented. The aim of this campaign is to estimate the polarimetric properties of asteroids belonging to the X taxonomic class. In this paper results of the campaign for M-type objects are presented. Methods: The data have been obtained with Casprof and Torino polarimeters at the 2.15 m telescope. The Casprof polarimeter is a two-hole aperture polarimeter with rapid modulation and the Torino polarimeter is an instrument that allows simultaneous measurement of polarization in the U-, B-, V-, R-, and I-bands. Results: The campaign began in 2000, and data on a sample of 26 M-type asteroids were obtained. Most of these objects were polarimetricaly observed for the first time. Combining these data with those available in the literature, an estimate of the polarimetric parameters and albedo for 12 objects is presented. Furthermore, the data show that asteroids 21 Lutetia and 77 Frigga have a large inversion angle and 441 Bathilde a deep polarization minimum, implying a controversial taxonomic classification as M-type for these objects. Also, the polarimetric parameters estimated for the M-type asteroids showing in their spectra the 3 μm band and classified as W-type by Rivkin et al. (1995, Icarus, 117, 90; 2000, ApJ, 145, 351) could be different from those without that feature. Based on observations carried out at the Complejo Astronómico El Leoncito, operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina, and the National Universities of La Plata, Córdoba and San Juan.

  19. Polarimetric survey of main-belt asteroids⋆. III. Results for 33 X-type objects

    Science.gov (United States)

    Cañada-Assandri, M.; Gil-Hutton, R.; Benavidez, P.

    2012-06-01

    Aims: We present results of a polarimetric survey of main-belt asteroids at Complejo Astronómico El Leoncito (Casleo), San Juan, Argentina. The aims of this survey are to increase the database of asteroid polarimetry, to estimate diversity in polarimetric properties of asteroids that belong to different taxonomic classes, and to search for objects that exhibit anomalous polarimetric properties. Methods: The data were obtained with the Torino and CASPROF polarimeters at the 2.15 m telescope. The Torino polarimeter is an instrument that allows the simultaneous measurement of polarization in five different bands, and the CASPROF polarimeter is a two-hole aperture polarimeter with rapid modulation. Results: The survey began in 2003, and up to 2009 data of a sample of more than 170 asteroids were obtained. In this paper the results for 33 X-type objects are presented, several of them are being polarimetrically observed for the first time. Using these data we found polarization curves and polarimetric parameters for different groups among this taxonomic class and that there are objects with very different albedo in the sub-classes of the X taxonomic complex. Based on observations carried out at the Complejo Astronómico El Leoncito, operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina and the National Universities of La Plata, Córdoba, and San Juan.Table 1 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/542/A11

  20. Variations of Synchrotron Radio Emissions from Jupiter's Inner Radiation Belt

    Science.gov (United States)

    Lou, Y.-Q.

    2017-09-01

    Variations of Synchrotron Radio Emissions from Jupiter's Inner Radiation Belt Yu-Qing Lou* Physics Department, Tsinghua Centre for Astrophysics (THCA), Tsinghua-National Astronomical Observatories of China (NAOC) joint Research Centre for Astrophysics, Tsinghua University, Beijing 100084, China We describe the basic phenommenology of quasi-periodic 40 minute (QP-40) polar burst activities of Jupiter and their close correlation with the solar wind speed variations at the Jovian magnetosphere. Physically, relativistic electrons of QP-40 bursts most likely come from the circumpolar regions of the inner radiation belt (IRB) which gives off intense synchroton radio emissions in a wide wavelength range. Such relativistic electron bursts also give rise to beamed low-frequency radio bursts along polar magnetic field lines with distinct polarizations from Jupiter's two polar regions. Jovian aurora activities are expected to be also affected by such QP-40 burst activities. We present evidence of short-term (typical timescales shorter than an hour) variabilities of the IRB at 6cm wavelength and describe recent joint radio telescope observation campaign to monitor Jupiter in coordination with JUNO spacecraft. Except for low-frequency polarization features, we anticipate JUNO to detect QP-40 activities from both polar regions during the arrival of high-speed solar wind with intermittency. References 1. Y.-Q. Lou, The Astrophysical Journal, 548, 460 (2001). 2. Y.-Q. Lou, and C. Zheng, Mon. Not. Roy. Astron. Soc. Letters, 344, L1 (2003). 3. Y.-Q. Lou, H. G. Song, Y.Y. Liu, and M. Yang, Mon. Not. Roy. Astron. Soc. Letters, 421, L62 (2012). 4. Y.-Q. Lou, Geophysical Research Letters, 23, 609 (1996). 5. Y.-Q. Lou, Journal of Geophysical Research, 99, 14747 (1994). 6. G. R. Gladstone, et al., Nature, 415, 1000 (2002).

  1. The extreme blazar AO 0235+164 as seen by extensive ground and space radio observations

    Science.gov (United States)

    Kutkin, A. M.; Pashchenko, I. N.; Lisakov, M. M.; Voytsik, P. A.; Sokolovsky, K. V.; Kovalev, Y. Y.; Lobanov, A. P.; Ipatov, A. V.; Aller, M. F.; Aller, H. D.; Lahteenmaki, A.; Tornikoski, M.; Gurvits, L. I.

    2018-01-01

    Clues to the physical conditions in radio cores of blazars come from measurements of brightness temperatures as well as effects produced by intrinsic opacity. We study the properties of the ultra compact blazar AO 0235+164 with RadioAstron ground-space radio interferometer, multi-frequency VLBA, EVN and single-dish radio observations. We employ visibility modeling and image stacking for deriving structure and kinematics of the source, and use Gaussian process regression to find the relative multi-band time delays of the flares. The multi-frequency core size and time lags support prevailing synchrotron self absorption. The intrinsic brightness temperature of the core derived from ground-based VLBI is close to the equipartition regime value. In the same time, there is evidence for ultra-compact features of the size of less than 10 μas in the source, which might be responsible for the extreme apparent brightness temperatures of up to 1014 K as measured by RadioAstron. In 2007-2016 the VLBI components in the source at 43 GHz are found predominantly in two directions, suggesting a bend of the outflow from southern to northern direction. The apparent opening angle of the jet seen in the stacked image at 43 GHz is two times wider than that at 15 GHz, indicating a collimation of the flow within the central 1.5 mas. We estimate the Lorentz factor Γ = 14, the Doppler factor δ = 21, and the viewing angle θ = 1.7° of the apparent jet base, derive the gradients of magnetic field strength and electron density in the outflow, and the distance between jet apex and the core at each frequency.

  2. Essays on Eclipses, Transits and Occultations as Teaching Tools in the Introductory Astronomy College Course. (Spanish Title: Ensayos sobre Eclipses, Tránsitos y Ocultaciones Como Herramientas de Enseñanza en el Curso Universitario Introductorio a la Astronomía.) Ensaios sobre Eclipses, Trânsitos e Ocultações Como Ferramentas de Ensino em um Curso Universitário Introdutório de Astromomia

    Science.gov (United States)

    Dcruz, Noella L.

    2014-07-01

    We occasionally include projects in our learner-centered introductory astronomy college course to enable non-science major students explore some astronomical concepts in more detail than otherwise. Such projects also highlight ongoing or upcoming astronomical events. We hope that students will feel more interested in astronomy through projects tied to astronomical events. In Spring 2012, we offered short essays focused on eclipses, transits and occultations to promote the rare transit of Venus that occurred on June 5th, 2012. We asked students to write two short essays from three that were offered. The essays contained descriptive and conceptual parts. They were meant to serve as teaching tools. 62% of 106 essays from 55 students earned A, B or C grades. 21% of 47 feedback survey respondents felt the essays increased their interest in astronomy. 49% of respondents felt that the essays were not educationally beneficial and should not be offered again. The most common written response to our survey indicated that students need more guidance and better preparation in writing successful essays. Since students found the conceptual parts of the essays difficult, in the future we will provide relevant activities prior to essay deadlines to help students create successful essays. Ocasionalmente, incluimos proyectos en nuestro curso de introducción a la astronomía universitario centrado en el alumno para permitir que los estudiantes de carreras no científicas exploren algunos conceptos astronómicos en más detalle que lo habitual. Estos proyectos también ponen en relevancia eventos astronómicos en curso o futuros. Esperamos que los estudiantes se sientan más interesados en la astronomía a través de proyectos vinculados a eventos astronómicos. En el período de primavera de 2012 (EUA), propusimos breves ensayos centrados en los eclipses, tránsitos y ocultaciones para promover el raro tránsito de Venus que se produjo el 5 de junio de 2012. Le pedimos a los

  3. Establishing the Empirical Relationship Between Non-Science Majoring Undergraduate Learners' Spatial Thinking Skills and Their Conceptual Astronomy Knowledge. (Spanish Title: Estableciendo Una Relación Empírica Entre el Razonamiento Espacial de los Estudiantes de Graduación de Carreras no Científicas y su Conocimento Conceptual de la Astronomía.) Estabelecendo Uma Relação Empírica Entre o RacioCínio Espacial dos Estudantes de Graduação EM Carreiras Não Científicas e Seu Conhecimento Conceitual da Astronomia

    Science.gov (United States)

    Heyer, Inge; Slater, Stephanie J.; Slater, Timothy F.

    2013-12-01

    The astronomy education community has tacitly assumed that learning astronomy is a conceptual domain resting upon spatial thinking skills. As a first step to formally identify an empirical relationship, undergraduate students in a non-major introductory astronomy survey class at a mediumsized, Ph.D. granting, mid-western US university were given pre- and post-astronomy conceptual diagnostics and spatial reasoning diagnostics, Instruments used were the "Test Of Astronomy Standards" and "What Do You Know?" Using only fully matched data for analysis, our sample consisted of 86 undergraduate non-science majors. Students' normalized gains for astronomy surveys were low at .26 and .13 respectively. Students' spatial thinking was measured using an instrument designed specifically for this study. Correlations between the astronomy instruments' pre- to post-course gain scores and the spatial assessment instrument show moderate to strong relationships suggesting the relationship between spatial reasoning and astronomy ability can explain about 25% of the variation in student achievement. La comunidad de educación en astronomía ha supuesto de forma tácita que el aprendizaje de la astronomía consiste en un dominio conceptual fundamentado en el razonamiento espacial. Como un primer paso para identificar formalmente una relación empírica entre estas dos cosas, utilizamos como muestra los estudantes de graduación de carreras no científicas de un curso experimental en una universidad norteamericana del medioeste de porte mediano con programa de Doctorado em curso, en el cual estos estudiantes se sometieron a un diagnóstico de razonamiento espacial y conceptos astronómicos antes e después del mismo. Las herramientas utilizadas fueron el Test Of Astronomy Standards (TOAST) y el cuestionario What do you know? Utilizando solo los datos completamente consistentes para este análisis, nuestra muestra consistió en 86 estudantes de graduación. Las mejoras, depués de

  4. The theory of canonical perturbations applied to attitude dynamics and to the Earth rotation. Osculating and nonosculating Andoyer variables

    Science.gov (United States)

    Efroimsky, Michael,; Escapa, Alberto

    2007-08-01

    In the method of variation of parameters we express the Cartesian coordinates or the Euler angles as functions of the time and six constants. If, under disturbance, we endow the “constants” with time dependence, the perturbed orbital or angular velocity will consist of a partial time derivative and a convective term that includes time derivatives of the “constants”. The Lagrange constraint, often imposed for convenience, nullifies the convective term and thereby guarantees that the functional dependence of the velocity on the time and “constants” stays unaltered under disturbance. “Constants” satisfying this constraint are called osculating elements. Otherwise, they are simply termed orbital or rotational elements. When the equations for the elements are required to be canonical, it is normally the Delaunay variables that are chosen to be the orbital elements, and it is the Andoyer variables that are typically chosen to play the role of rotational elements. (Since some of the Andoyer elements are time-dependent even in the unperturbed setting, the role of “constants” is actually played by their initial values.) The Delaunay and Andoyer sets of variables share a subtle peculiarity: under certain circumstances the standard equations render the elements nonosculating. In the theory of orbits, the planetary equations yield nonosculating elements when perturbations depend on velocities. To keep the elements osculating, the equations must be amended with extra terms that are not parts of the disturbing function [Efroimsky, M., Goldreich, P.: J. Math. Phys. 44, 5958 5977 (2003); Astron. Astrophys. 415, 1187 1199 (2004); Efroimsky, M.: Celest. Mech. Dyn. Astron. 91, 75 108 (2005); Ann. New York Acad. Sci. 1065, 346 374 (2006)]. It complicates both the Lagrange- and Delaunay-type planetary equations and makes the Delaunay equations noncanonical. In attitude dynamics, whenever a perturbation depends upon the angular velocity (like a switch to a

  5. Corrections stemming from the non-osculating character of the Andoyer variables used in the description of rotation of the elastic Earth

    Science.gov (United States)

    Escapa, Alberto

    2011-06-01

    We explore the evolution of the angular velocity of an elastic Earth model, within the Hamiltonian formalism. The evolution of the rotation state of the Earth is caused by the tidal deformation exerted by the Moon and the Sun. It can be demonstrated that the tidal perturbation to spin depends not only upon the instantaneous orientation of the Earth, but also upon its instantaneous angular velocity. Parameterizing the orientation of the Earth figure axis with the three Euler angles, and introducing the canonical momenta conjugated to these, one can then show that the tidal perturbation depends both upon the angles and the momenta. This circumstance complicates the integration of the rotational motion. Specifically, when the integration is carried out in terms of the canonical Andoyer variables (which are the rotational analogues to the orbital Delaunay variables), one should keep in mind the following subtlety: under the said kind of perturbations, the functional dependence of the angular velocity upon the Andoyer elements differs from the unperturbed dependence (Efroimsky in Proceedings of Journées 2004: Systèmes de référence spatio-temporels. l'Observatoire de Paris, pp 74-81, 2005; Efroimsky and Escapa in Celest. Mech. Dyn. Astron. 98:251-283, 2007). This happens because, under angular velocity dependent perturbations, the requirement for the Andoyer elements to be canonical comes into a contradiction with the requirement for these elements to be osculating, a situation that parallels a similar antinomy in orbital dynamics. Under the said perturbations, the expression for the angular velocity acquires an additional contribution, the so called convective term. Hence, the time variation induced on the angular velocity by the tidal deformation contains two parts. The first one comes from the direct terms, caused by the action of the elastic perturbation on the torque-free expressions of the angular velocity. The second one arises from the convective terms. We

  6. Impact and cratering rates onto Pluto

    Science.gov (United States)

    Greenstreet, Sarah; Gladman, Brett; McKinnon, William B.

    2015-09-01

    The New Horizons spacecraft fly-through of the Pluto system in July 2015 will provide humanity's first data for the crater populations on Pluto and its binary companion, Charon. In principle, these surfaces could be dated in an absolute sense, using the observed surface crater density (# craters/km2 larger than some threshold crater diameter D). Success, however, requires an understanding of both the cratering physics and absolute impactor flux. The Canada-France Ecliptic Plane Survey (CFEPS) L7 synthetic model of classical and resonant Kuiper belt populations (Petit, J.M. et al. [2011]. Astron. J. 142, 131-155; Gladman, B. et al. [2012]. Astron. J. 144, 23-47) and the scattering object model of Kaib et al. (Kaib, N., Roškar, R., Quinn, T. [2011]. Icarus 215, 491-507) calibrated by Shankman et al. (Shankman, C. et al. [2013]. Astrophys. J. 764, L2-L5) provide such impact fluxes and thus current primary cratering rates for each dynamical sub-population. We find that four sub-populations (the q 100km) connects to smaller projectiles, we compute cratering rates using five model impactor size distributions: a single power-law, a power-law with a knee, a power-law with a divot, as well as the "wavy" size distributions described in Minton et al. (Minton, D.A. et al. [2012]. Asteroids Comets Meteors Conf. 1667, 6348) and Schlichting et al. (Schlichting, H.E., Fuentes, C.I., Trilling, D.E. [2013]. Astron. J. 146, 36-42). We find that there is only a small chance that Pluto has been hit in the past 4 Gyr by even one impactor with a diameter larger than the known break in the projectile size distribution (d ≈ 100km) which would create a basin on Pluto (D ⩾ 400km in diameter). We show that due to present uncertainties in the impactor size distribution between d = 1- 100km , computing absolute ages for the surface of Pluto is entirely dependent on the extrapolation to small sizes and thus fraught with uncertainty. We show, however, what the ages would be for several cases

  7. Modelo numérico tri-dimensional linear da plataforma continental do Estado do Maranhão Linear three-dimensional numerical model of Maranhão State continental shelf

    Directory of Open Access Journals (Sweden)

    José Edson Rodrigues Pereira

    1995-01-01

    Full Text Available Um modelo numérico hidrodinámico tri-dimensional linear, do tipo Heaps, foi implementado para a plataforma continental do Estado do Maranhão, visando a simulação da circulação gerada por efeitos astronômicos e meteorológicos na área. O modelo foi processado para cinco condições, a fim de calcular a circulação na plataforma devida aos seguintes efeitos: componente de maré semi-diurna lunar principal (M2, composição das principais componentes astronômicas de maré na área, condições meteorológicas médias de verão, condições meteorológicas médias de inverno e forçantes de maré em períodos específicos de interesse. Mapas cotidais e elipses de correntes da componente M2 foram obtidos, sendo esta componente preponderante na circulação local. Elevações e correntes sazonais médias são, em geral, muito menores que as astronômicas, permitindo o uso apenas de forçantes de maré em previsões hidrodinámicas. As simulações do modelo foram satisfatórias na plataforma e menos precisas nas baías e áreas internas rasas, onde atrasos de fase significativos são observados, devido a efeitos de menor escala que a adotada pelo modelo.A linear three-dimensional hydrodynamical numerical model, Heaps type, was implemented to the continental shelf of Maranhão State, aiming the simulation of the circulation generated by astronomical and meteorological effects in that area. Five runs of the model were performed, in order to compute the circulation in the shelf due to the following effects: principal lunar semi-diurnal component (M2, composition of the principal astronomical components in the area, mean summer meteorological conditions, mean winter meteorological conditions and tidal forcing in specific periods of interest. M2 cotidal maps and currents ellipses were obtained, that one being the most important component in the tidal circulation. Mean seasonal elevations and currents are generally much smaller than the

  8. Origin and Evolution of the Cometary Reservoirs

    Science.gov (United States)

    Dones, Luke; Brasser, Ramon; Kaib, Nathan; Rickman, Hans

    2015-12-01

    underwent a dynamical instability that led to a flood of comets and asteroids throughout the Solar System (Gomes et al. in Nature 435:466-469, 2005b). In this scenario, it is somewhat a matter of luck whether an icy planetesimal ends up in the Kuiper Belt or Oort Cloud (Brasser and Morbidelli in Icarus 225:40-49, 2013), as a Trojan asteroid (Morbidelli et al. in Nature 435:462-465, 2005; Nesvorný and Vokrouhlický in Astron. J. 137:5003-5011, 2009; Nesvorný et al. in Astrophys. J. 768:45, 2013), or as a distant "irregular" satellite of a giant planet (Nesvorný et al. in Astron. J. 133:1962-1976, 2007). Comets could even have been captured into the asteroid belt (Levison et al. in Nature 460:364-366, 2009). The remarkable finding of two "inner Oort Cloud" bodies, Sedna and 2012 VP_{113}, with perihelion distances of 76 and 81 AU, respectively (Brown et al. in Astrophys. J. 617:645-649, 2004; Trujillo and Sheppard in Nature 507:471-474, 2014), along with the discovery of other likely inner Oort Cloud bodies (Chen et al. in Astrophys. J. Lett. 775:8, 2013; Brasser and Schwamb in Mon. Not. R. Astron. Soc. 446:3788-3796, 2015), suggests that the Sun formed in a denser environment, i.e., in a star cluster (Brasser et al. in Icarus 184:59-82, 2006, 191:413-433, 2007, 217:1-19, 2012b; Kaib and Quinn in Icarus 197:221-238, 2008). The Sun may have orbited closer or further from the center of the Galaxy than it does now, with implications for the structure of the Oort Cloud (Kaib et al. in Icarus 215:491-507, 2011).

  9. THE POPULARIZATION OF ASTRONOMY IN THE TEACHING OF GEOGRAPHY: an experience in the middle and high school

    Directory of Open Access Journals (Sweden)

    Márcio Balbino Cavalcante

    2012-12-01

    Full Text Available It is a very old man's concern to know the mysteries of the universe. Geography is defined as the study of the relationship between space and society, is, par excellence, discipline and interdisciplinary teaching should focus on various aspects of society and nature. The present study was aimed to popularize astronomy in Geography lessons of elementary and secondary public and private schools of the municipality the of Passa e Fica/RN, with reference to the achievement of the Olympiad of Astronomy and Astronautics - OBA, sponsored by the Institute Physics - UERJ in partnership with the Sociedade Astronômica Brasileira (SAB and the Agência Espacial Brasileira (AEB. The achievement of this Article, the following steps were undertaken: literature search and mapping, field survey;-class ride to Centro de Lançamento de Foguetes da Barreira do Inferno, em Natal/RN; lectures, telescopic observations, workshops for carrying out activities practices such as the sundial, replica rocket, compass; classroom discussion of the data collected, the material made with exposure and mobilization involving the school community and the Government. According to the results, interdisciplinary work between geography and astronomy produced a privileged space for the construction and popularization of scientific knowledge founded on the reality experienced by the student, always with a critical and constructive, which often is ignored in school work. RESUMO: É muito antiga a preocupação do homem em conhecer os mistérios do universo. A Geografia é definida como o estudo das relações entre o espaço e as sociedades, é, por excelência, uma disciplina interdisciplinar e seu ensino deve enfocar diversos aspectos da sociedade e da natureza. O presente trabalho teve objetivo de popularizar a Astronomia nas aulas de Geografia dos ensinos fundamental e médio das escolas públicas e particulares do município de Passa e Fica/RN; tendo como referência a realiza

  10. Deciphering the embedded wave in Saturn's Maxwell ringlet

    Science.gov (United States)

    French, Richard G.; Nicholson, Philip D.; Hedman, Mathew M.; Hahn, Joseph M.; McGhee-French, Colleen A.; Colwell, Joshua E.; Marouf, Essam A.; Rappaport, Nicole J.

    2016-11-01

    The eccentric Maxwell ringlet in Saturn's C ring is home to a prominent wavelike structure that varies strongly and systematically with true anomaly, as revealed by nearly a decade of high-SNR Cassini occultation observations. Using a simple linear "accordion" model to compensate for the compression and expansion of the ringlet and the wave, we derive a mean optical depth profile for the ringlet and a set of rescaled, background-subtracted radial wave profiles. We use wavelet analysis to identify the wave as a 2-armed trailing spiral, consistent with a density wave driven by an m = 2 outer Lindblad resonance (OLR), with a pattern speed Ωp = 1769.17° d-1 and a corresponding resonance radius ares = 87530.0 km. Estimates of the surface mass density of the Maxwell ringlet range from a mean value of 11g cm-2 derived from the self-gravity model to 5 - 12gcm-2 , as inferred from the wave's phase profile and a theoretical dispersion relation. The corresponding opacity is about 0.12 cm2 g-1, comparable to several plateaus in the outer C ring (Hedman, M.N., Nicholson, P.D. [2014]. Mont. Not. Roy. Astron. Soc. 444, 1369-1388). A linear density wave model using the derived wave phase profile nicely matches the wave's amplitude, wavelength, and phase in most of our observations, confirming the accuracy of the pattern speed and demonstrating the wave's coherence over a period of 8 years. However, the linear model fails to reproduce the narrow, spike-like structures that are prominent in the observed optical depth profiles. Using a symplectic N-body streamline-based dynamical code (Hahn, J.M., Spitale, J.N. [2013]. Astrophys. J. 772, 122), we simulate analogs of the Maxwell ringlet, modeled as an eccentric ringlet with an embedded wave driven by a fictitious satellite with an OLR located within the ring. The simulations reproduce many of the features of the actual observations, including strongly asymmetric peaks and troughs in the inward-propagating density wave. We argue that

  11. Proving the Orbits of the Galilean Moons Through Astrophotography. (Spanish Title: Comprobando Las Órbitas de Las Lunas Galileanas a Través de la Astrofotografía.) Evidenciando as Órbitas das Luas Galileanas Atravéd da Astrofotografia

    Science.gov (United States)

    Iachel, Gustavo

    2009-12-01

    An activity related to the observation of the Galilean moons and to amateur astrophotography is presented in this work. Through the reading of excerpts of the book Sidereus Nuncius (Sidereal Messenger), by Galileo, it is possible to trace a methodology to observe the planet and its natural satellites and, with the aid of the astrophotography, to analyze the field recordings. Moreover, it is possible to compare the images obtained after plotting the relative positions of these moons to prove their orbits. This activity can be conducted by teachers, students and amateur astronomers, in order to develop their capabilities of observation of astronomical phenomena. Se presenta en este trabajo una actividad relacionada a la observación de las lunas Galileanas y a la astrofotografía amateur. A través de la lectura de tramos de la obra Sidereus Nuncius (El Mensajero Sideral) de Galileo, es posible trazar una metodología para la observación del planeta y de sus satélites naturales y, con el auxilio de la astrofotografía, analizar las anotaciones de campo. Además, es posible comparar las imágenes obtenidas con el gráfico de las posiciones relativas de estas lunas para comprobar sus órbitas. Esa actividad puede ser realizada por maestros, estudiantes y astrónomos amateurs, de forma a desarrollar sus capacidades de observación de los fenómenos astronómicos. Uma atividade relacionada à observação das luas Galileanas e à astrofotografia amadora é apresentada neste trabalho. Através da leitura de trechos da obra Sidereus Nuncius (Mensageiro Sideral), de Galileu, é possível traçar uma metodologia para a observação do planeta e de seus satélites naturais e, com o auxílio da astrofotografia, analisar as anotações de campo. Além disso, é possível comparar as imagens obtidas com o gráfico das posições relativas destas luas para evidenciar suas órbitas. Essa atividade pode ser realizada por professores, estudantes e astrônomos amadores, de forma a

  12. Asteroid Families: Myth or Reality?

    Science.gov (United States)

    Bus, S. J.; Binzel, R. P.; Burbine, T. H.

    1996-09-01

    Dynamical families among the asteroids are thought to result from the collisional disruption of larger parent bodies. Even with recent improvements in the calculation of proper elements and the use of better clustering algorithms, a grouping in orbital element space is not sufficient proof of a genetic association. Proof of a genetic link between these objects is possible only through physical studies of the individual family members. In the course of the Small Main-Belt Asteroid Spectroscopic Survey (SMASS), we have measured the spectral reflectance properties of more than 250 asteroids whose semi-major axes are between 2.7 and 2.82 AU. This region of the main-belt has been chosen for study due to the diversity of asteroid spectral types present, and for the number of dynamical families that have been identified (e.g., Williams 1992, Icarus 96, 251 and Zappala et al. 1994, Astron. J. 107, 772). We have focused our efforts on 10 families defined by Zappala et al. (1995, Icarus 116, 291) (Astrid, Ceres, Chloris, Dora, Henan, Hoffmeister, Liberatrix, Lydia, Merxia, Nemesis) and on the proposed high inclination Pallas family (e.g., Lemaitre and Morbidelli 1994, Cel. Mech. Dynam. Astron. 60, 29). Observations were obtained with a CCD spectrograph attached to the 2.4-m Hiltner telescope of the Michigan-Dartmouth-MIT Observatory and cover the wavelength range of 4400-9200 Angstroms. Of the >250 objects observed, approximately one-half are identified as family members while the other half are non-family members, where the latter are used to define the background population. For each of the eleven families studied, strong similarities are seen in the reflectance properties between the individual family members. This is in significant contrast to the relatively random distribution of C-type and S-type asteroids seen in the background population. Interlopers are found, but usually appear to be at the periphery of a family, highlighting the difficulty of establishing

  13. Light scattering observations and simulations, as hints about the media encountered by future rendezvous missions to comets and asteroids

    Science.gov (United States)

    Levasseur-Regourd, Anny-Chantal

    contribute to the success of future space missions. [1] Levasseur-Regourd and Hadamcik, J. Quant. Spectros. Radiat. Transfer 79, 903-910, 2003. [2] Pentill¨ et al., Astron. Astrophys. 432, 1081-1090, 2005. [3] Levasseur-Regourd a et al., Astron. Astrophys. 313, 327-333, 1996. [4] Lasue and Levasseur-Regourd, J. Quant. Spectros. Radiat. Transfer 100, 220-236, 2006. [5] Hadamcik et al., Icarus 190, 660-671, 2007. [6] Levasseur-Regourd et al., Planet. Space Sci. 55, 1010-1020, 2007. [7] H¨rz et al., Science o 314, 1716-1719 (2006).

  14. Visibility retrieval in Michelson wide-field stellar interferometry

    Science.gov (United States)

    Montilla, I.; Sellos, J.; Pereira, S. F.; Braat, J. J. M.

    2006-04-01

    Wide-field interferometry has become a subject of increasing interest in recent years. New methods have been suggested in order to avoid the drawbacks of the standard wide-field method (homothetic mapping), which is not applicable when the aperture is highly diluted; for this reason, imaging with non-homothetic arrays is being extensively studied (E. Pedretti, et al., Astron. Astrophys. Suppl. Ser. 147 285 (2000); S. Gillet, et al., Astron. Astrophys. 400 393 (2003)). The field of view of a pupil-plane interferometer or a densified array consists of only a few resolution elements; in order to improve these systems, we have developed a new method consisting of a Michelson pupil-plane combination scheme where a wide field of view can be achieved in one shot. This technique, called the ‘staircase mirror’ approach, has been described in a previous paper (I. Montilla, S.F. Pereira and J.J.M. Braat, Appl. Optics 44 328 (2005)) and uses a stair-shaped mirror in the intermediate image plane of each telescope in the array, allowing for simultaneous correction of the differential delay for both the on- and off-axis image positions. Experimental results have been obtained showing the simultaneous recovery of the fringes of off-axis stars with an appreciable angular separation, and with a contrast similar to that of the on-axis reference star. With this example we demonstrate an increase of the field of view by a factor of 5, with no need for extra observation time. In this article, we present a further analysis of the method. We investigate how to retrieve the visibility when a star is focused on the edge of a step of the stair-shaped mirror. Even though the optical pathlength difference correction is discontinuous, we show both numerically and analytically that the visibility can be completely recovered, so that no information is lost. Our experimental results demonstrate that the visibility can be retrieved to within a 1% error.

  15. Polarimetric survey of main-belt asteroids. VI. New results from the second epoch of the CASLEO survey

    Science.gov (United States)

    Gil-Hutton, R.; García-Migani, E.

    2017-11-01

    Aims: We present the results of a polarimetric survey of main-belt asteroids at Complejo Astronómico El Leoncito (CASLEO), San Juan, Argentina. The aims of this survey are to increase the database of asteroid polarimetry and to estimate the diversity in the polarimetric properties of asteroids that belong to different taxonomic classes. Methods: The data were obtained using the CASPOL polarimeter at the 2.15 m telescope. CASPOL is a polarimeter based on a CCD detector and a Savart plate. The survey began in 1995 and data on a large sample of asteroids were obtained until 2012. A second period began in 2013 using a polarimeter with a more sensitive detector in order to study small asteroids, families, and special taxonomic groups. Results: We present and analyze the unpublished results for 128 asteroids of different taxonomic types, 55 of them observed for the first time. The observational data allowed us to find probable new cases of Barbarian objects but also two D-type objects, (565) Marbachia and (1481) Tubingia, that seem to have phase-polarization curves with a large inversion angle. The data obtained combined with data from the literature enabled us to find phase-polarization curves for 121 objects of different taxonomic types and to study the relations between several polarimetric and physical parameters. Using an approximation for the phase-polarization curve we found the index of refraction of the surface material and the scatter separation distance for all the objects with known polarimetric parameters. We also found that the inversion angle is a function of the index of refraction of the surface, while the phase angle where the minimum of polarization is produced provides information about the distance between scatter particles or, to some extent, the porosity of the surface. Based on observations carried out at the Complejo Astronómico El Leoncito, operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la

  16. The Teaching of Astronomy in Uruguay. (Spanish Title: La Enseñanza de la Astronomía en Uruguay.) O Ensino da Astronomia no Uruguai

    Science.gov (United States)

    Pintos Ganón, Reina; Fernández, Julio Angel

    2008-07-01

    We present in this work the development of astronomy in Uruguay since the colony times up to the present, stressing in particular those aspects related to the formal as well as informal teaching of astronomy. The first antecedents of astronomical studies in our country go back to the beginnings of the XVIIIth century related to the scientific expeditions from Europe coming to our shores. The teaching of astronomy was generalized at the high school level as soon as the end of the XIXth century, while itsintroduction at the university level happened much later, around the middle of the last century. We analyze the current situation of this subject, its problems, and some measures to strengthen its development. Se presenta en este trabajo el desarrollo de la astronomía en el Uruguay desde la época colonial hasta el presente, destacando en particular los aspectos vinculados a su enseñanza tanto formal como informal. Los primeros antecedentes de estudios astronómicos datan de la época colonial relacionados con las expediciones científicas del Viejo Mundo que llegaban a nuestras costas. La enseñanza de la Astronomía se generalizó en el ámbito de los estudios secundarios ya a fines del siglo XIX, mientras que en la Universidad su arribo fue mucho más tardío, a mediados del siglo pasado. Se analiza la situación actual de esta disciplina, sus problemas, y algunas medidas para fortalecer su desarrollo. Apresentamos, neste trabalho, o desenvolvimento da Astronomia no Uruguai desde a época colonial até o presente, destacando em particular os aspectos vinculados ao seu ensino tanto formal quanto informal. Os primeiros antecedentes de estudos astronômicos em nosso país datam da época colonial relacionados com as expedições científicas do Velho Mundo que chegavam às nossas costas. O ensino da Astronomia se generalizou no âmbito dos estudos secundários já no final do século XIX, enquanto que sua introdução na universidade foi muito mais tardia, em

  17. Planetesimal-driven planet migration in the presence of a gas disk

    Science.gov (United States)

    Capobianco, Christopher C.; Duncan, Martin; Levison, Harold F.

    2011-01-01

    We report here on an extension of a previous study by Kirsh et al. (Kirsh, D.R., Duncan, M., Brasser, R., Levison, H.F. [2009]. Icarus 199, 197-209) of planetesimal-driven migration using our N-body code SyMBA (Duncan, M.J., Levison, H.F., Lee, M.H. [1998]. Astron. J. 116, 2067-2077). The previous work focused on the case of a single planet of mass Mem, immersed in a planetesimal disk with a power-law surface density distribution and Rayleigh distributed eccentricities and inclinations. Typically 10 4-10 5 equal-mass planetesimals were used, where the gravitational force (and the back-reaction) on each planetesimal by the Sun and planet were included, while planetesimal-planetesimal interactions were neglected. The runs reported on here incorporate the dynamical effects of a gas disk, where the Adachi et al. (Adachi, I., Hayashi, C., Nakazawa, K. [1976]. Prog. Theor. Phys. 56, 1756-1771) prescription of aerodynamic gas drag is implemented for all bodies. In some cases the Papaloizou and Larwood (Papaloizou, J.C.B., Larwood, J.D. [2000]. Mon. Not. R. Astron. Soc. 315, 823-833) prescription of Type-I migration for the planet are implemented, as well as a mass distribution. In the gas-free cases, rapid planet migration was observed - at a rate independent of the planet's mass - provided the planet's mass was not large compared to the mass in planetesimals capable of entering its Hill sphere. In such cases, both inward and outward migrations can be self-sustaining, but there is a strong propensity for inward migration. When a gas disk is present, aerodynamic drag can substantially modify the dynamics of scattered planetesimals. For sufficiently large or small mono-dispersed planetesimals, the planet typically migrates inward. However, for a range of plausible planetesimal sizes (i.e. 0.5-5.0 km at 5.0 AU in a minimum mass Hayashi disk) outward migration is usually triggered, often accompanied by substantial planetary mass accretion. The origins of this behaviour are

  18. Los modelos etnomatemáticos de representación cosmogónica en los pueblos indígenas Americanos

    Directory of Open Access Journals (Sweden)

    Alejandro Jaén Rojas

    2015-01-01

    Full Text Available El propósito en este artículo es el de mostrar y analizar diversas formas de representación que utilizaron o, utilizan aun los indígenas americanos de diversas culturas. Algunas formas de representación, consideradas comúnmente como motivos decorativos, parecen responder a un sistema lógico muy preciso, que podría tener el propósito central de expresar y guardar conocimientos cosmogónicos. Para tal efecto, los indígenas de diversos pueblos, recurrieron a estructuras y formas de representación matemáticas, que les permitían guardar conocimientos astronómicos, calendáricos, de las cosechas, censos, entre otros, y luego expresarlos como mitos, integrados dentro de su espacio cosmogónico. Resulta sorprendente ver como algunas formas de representación, como las grecas escalonadas, pasan de una cultura a otra, desde Alaska hasta la Patagonia, en lo que parecen ser modelos de representación, que se difundieron muchos siglos antes de la llegada de los españoles a América. La razón por la cual, estos modelos de representación se generalizan, a lo largo de distancias enormes y entre los pueblos más diversos, es porque son conocimientos que surgen ligados a los tejidos. Hasta donde sabemos, casi la totalidad de los indígenas tejían en algodón o diversas fibras, con lo cual, una vez iniciado el proceso de guardar informaciones todos ellos contaron con una base simple y sólida para fortalecer el proceso de recopilación de datos, y guardarlos con precisión. Muchos son los ejemplos de cómputos realizados con mecates, al estilo de los quipus suramericanos. En el arte de tejer surgen conocimientos matemáticos que les permitieron guardar informaciones muy variadas: calendáricas, astronómicas, culturales, entre otras, que luego eran expresadas como una visión de mundo, una cosmogonía.

  19. Taxonomía de asteroides y cometas basada en los espectros de Lyapunov

    Science.gov (United States)

    Tancredi, G.; Motta, V.; Froeschlé, C.

    Estudiaremos dos familias de objetos que sufren encuentros cercanos con planetas, a saber: la familia de cometas de Júpiter (JF) y los asteroides cercanos a la Tierra (NEAs). El movimiento de estos objetos es caótico en una escala de tiempo corta. Más aún, debido a los cambios erráticos en los elementos orbitales, la comparación de los valores actuales da poca información acerca de la posible vinculación dinámica entre los objetos de una misma familia. Calculamos una estimación finita de los Exponentes Característicos de Lyapunov (LCE), los llamamos Indicadores Característicos de Lyapunov (LCI) para ambas familias y analizamos las características del espacio de fase donde tiene lugar el movimiento de estos objetos. Integrando en un período suficientemente largo (e.g. 20000 años), encontramos que el LCI alcanza un valor cuasi-constante. La mayoría de los miembros de ambas familias muestran una concentración de los tiempos de Lyapunov (inverso del LCI) de alrededor de 50-100 años (Tancredi, 1995, Astron & Astrop., 299, 288). La concentración de los tiempos de Lyapunov es mayor para la familia de Júpiter que para los NEAs. Entre estos últimos, la menor dispersión se da para aquellos que cruzan la órbita de la Tierra. Se demostró que el espectro de los `indicadores locales' (Froeschlé et. al., 1990, Cel. Mec. 56, 307) o ``números de estiramiento'' (Voglis and Contopoulos, 1994, J. Phys. A 26, 4899) (relacionados con el LCI) son invariantes y nos dan una información más completa sobre el comportamiento caótico. Mediante la comparación de espectros discutimos la similitud entre los objetos de una misma familia y analizamos las diferentes posibles rutas al caos. Los espectros se clasifican mediante la comparación de los momentos de las distribuciones de los `números de estiramiento'. Aplicamos un método de agrupamiento jerárquico (Zappala et. al., 1990, Astron. J. 100, 2030) para identificar ``familias'' de espectros (grupos de espectros

  20. Monitoreo del Clima Espacial desde Colombia mediante Radio-receptores Butterworth de Orden Superior

    Directory of Open Access Journals (Sweden)

    Andrés Felipe Jaramillo Alvarado

    2017-01-01

    Full Text Available Contexto: las fulguraciones solares y las eyecciones de masa coronal liberan al espacio grandes cantidades de radiación que, al alcanzar las capas exteriores de la atmósfera terrestre, alteran sus características eléctricas. El conjunto de fenómenos derivados de esta interacción se conoce como clima espacial y sus consecuencias incluyen fallas en los sistemas de geolocalización, las telecomunicaciones, las operaciones vía satélite, el seguimiento espacial, la radionavegación y la sobrecarga de redes eléctricas. Método: en este trabajo se presenta el desarrollo de un radio receptor que permite adelantar el monitoreo del clima espacial desde Colombia. Además, se describe una metodología novedosa para el diseño de filtros analógicos de orden superior de característica Butterworth, a partir de la interconexión en paralelo de bancos de filtros de primero y segundo orden, obteniéndose la función de transferencia deseada. Resultados: el radio receptor desarrollado se instaló en la estación de monitoreo del clima espacial del Observatorio Astronómico de la Universidad Tecnológica de Pereira (OAUTP, Colombia, entrando en operación en diciembre de 2015. Desde esa fecha, el sistema ha registrado la actividad solar de forma ininterrumpida, detectando cuatro potentes explosiones solares clase C presentadas los días 15, 16 y 17 del mes de abril de 2016. Las señales recibidas por el radio receptor son enviadas a la base de datos global del Stanford Solar Center, de Stanford University, con el código UTP 0383. Conclusiones: el radio telescopio desarrollado permite al Observatorio Astronómico OAUTP adelantar el monitoreo del clima espacial y de la actividad solar, enviando la información recibida a repositorios de acceso público a nivel mundial. No existen otros receptores de radio de este tipo operando en la actualidad en países ecuatoriales, una región de la Tierra donde los efectos de la actividad solar pueden conducir a

  1. Cálculo da latitude e direção dos pólos pela projeção da trajetória circular das estrelas

    Directory of Open Access Journals (Sweden)

    Julierme Wagner da Penha

    2009-08-01

    Full Text Available Muitas vezes, a gente olha para o céu e admira a beleza das estrelas, até contamos, mas nem imaginamos que podemos estudar estes astros luminosos, bem como nos localizarmos por meio deles, assim como faziam os navegadores do passado. Na verdade, esta atividade é uma das mais antigas estudadas pelo homem. Este trabalho mostra um método novo e simplificado para determinar tanto a coordenada da latitude astronômica e a direção do Pólo Norte ou do Sul, por meio da observação de estrelas. A idéia é que esse método possa ser utilizado sem a prévia informação do anuário astronômico, bem como sem a prévia escolha do astro a ser observado. O método tem originado do princípio de que, caso tivéssemos um astro localizado exatamente na posição do pólo sul, seria suficiente posicionar o instrumento e visar o astro para determinar a latitude (altura do pólo elevado, independentemente do horário de observação, pois, o mesmo não teria movimento aparente algum. Portanto, este método sugere que, após a escolha do astro, o mesmo deverá ser observado, no mínimo em três posições diferentes. Projetando estas trajetórias em um plano perpendicular ao eixo terrestre rotação da Terra no pólo, tem-se várias circunferências concêntricas. O centro desta circunferência seria a posição exata do pólo. Determinando o centro da circunferência determina-se também a latitude e a direção dos pólos. Pode-se concluir que o método apresentado é viável para determinação da latitude e da direção dos pólos, pois os resultados encontrados foram satisfatórios.

  2. Astronomy Teaching and Teachers Continuing Education: the Interdisciplinarity during a Total Lunar Eclipse. (Spanish Title: Enseñanza de la Astronomía y la Formación Continua de Profesores: la Interdisciplinariedad Durante un Eclipse Total de Luna.) Educação EM Astronomia E Formação Continuada de Professores: a Interdisciplinaridade Durante um Eclipse Lunar TOTAL

    Science.gov (United States)

    Langhi, Rodolfo

    2009-07-01

    This paper describes how 67 teachers from 23 cities, could awaken, in students, the scientific interest, using a natural astronomical phenomenon: a total lunar eclipse. Before and after of eclipse, meetings for continuing education were characterized by interdisciplinarity of astronomy and the importance of these observations. Working groups were formed by teachers and students, who organized the survey data, mobilizing the people in their cities. The results point ways about how to provide the scientific culture and the motivation to learn science in students, using approaches between the following communities: scientific, amateur and school. En este artículo se describe cómo 67 profesores de 23 ciudades, despertó el interés científico en los estudiantes mediante un fenómeno astronómico: un eclipse total de Luna. Antes y después del eclipse, reuniones para la formación continua se centraron en la interdisciplinariedad de la astronomía, y la importancia de las observaciones de este tipo de fenómeno. Profesores y estudiantes formaron grupos de trabajo para investigar datos durante el eclipse, con el participación de la comunidad en sus ciudades. Los resultados apuntan a las opciones que conducen a la cultura científica y la motivación para aprender la ciencia, utilizando las relaciones de los siguientes grupos: científicos, aficionados y la escuela. Este texto relata como 67 professores, provenientes de 23 cidades, puderam despertar, nos alunos, o interesse científico utilizando um fenômeno natural astronômico: um eclipse lunar total. O evento foi precedido e procedido por encontros de formação continuada, onde se caracterizou a interdisciplinaridade da astronomia e a importância das observações de fenômenos como estes. Grupos de trabalho foram formados por professores e alunos, que se organizaram para o levantamento conjunto de dados durante o fenômeno, além do envolvimento da comunidade em suas respectivas cidades. Os resultados apontam

  3. From 9 to 12 and Finally 8: how Many Planets are around the Sun? (Spanish Title: De 9 a 12 y Finalmente 8: ¿Cuántos Planetas Hay Alrededor del Sol?) De 9 a 12 e Finalmente 8: Quantos Planetas Existem AO Redor do Sol?

    Science.gov (United States)

    Tancredi, Gonzalo

    2007-12-01

    The International Astronomical Union, the organization that groups together the professional astronomers over the world, has recently adopted a historical definition: What is a planet in the Solar System? Changing 76 years of tradition, our Solar System has now 8 planets and an increasing number of a new category of bodies named "dwarf planets", among them is the former planet Pluto. In this article we present the reasons that support the resolution and we describe the participation of the Latin-American astronomers in the process to adopt it. La Unión Astronómica Internacional, la organización que agrupa a los astrónomos profesionales del planeta, acaba de adoptar una definición histórica: ¿Qué es un planeta en nuestro Sistema Solar? Cambiando 76 años de tradición, según esta definición, nuestro Sistema Solar cuenta con 8 planetas y una creciente cantidad de "planetas enanos", entre los que quedó incluido el hasta hace poco planeta Plutón. En el presente artículo se presentarán los argumentos que fundamentan esta resolución y la participación que han tenido los astrónomos latinoamericanos en la adopción de la misma. A União Astronômica Internacional, a organização que agrupa os astrônomos profissionais do planeta, acaba de adotar uma definição histórica: O que é um planeta em nosso Sistema Solar? Mudando 76 anos de tradição, segundo esta definição, nosso Sistema Solar conta com 8 planetas e uma crescente quantidade de "planetas anões", entre os quais foi incluido o até há pouco planeta Plutão. No presente artigo serão apresentados os argumentos que fundamentam esta resolução e a participação que tiveram os astrônomos latino-americanos na adoção da mesma.

  4. Ensino de astronomia e óptica: é possível fazê-lo de forma contextualizada no nível médio?

    Science.gov (United States)

    Sobrinho, A. A.; Jafelice, L. C.

    2003-08-01

    Discutimos nossa participação em um curso de treinamento para professores de diversas disciplinas do ensino médio. Nossa preocupação básica foi desenvolver instrumentos educacionais adequados para levar à sala de aula, nesse nível de ensino, de forma contextualizada, questionamentos freqüentes dos alunos sobre astronomia e sua relação com tecnologia e sociedade. Encaminhamos questões como: a evolução da astronomia, suas relações com outros ramos do conhecimento humano e conseqüentes aplicações; avanços na tecnologia dos instrumentos ópticos versus a importância da observação do céu a olho nu; a relação entre olho humano, luneta e telescópio; e desenvolvimento da tecnologia espacial e sua influência em nosso cotidiano. Objetivamos com isto fazer um resgate histórico e pedagógico das aplicações e observações do céu no cenário escolar, destacando a relação entre eventos astronômicos, olho humano, instrumentos mediadores e suas contextualizações históricas e sociais. Produtos desta abordagem foram o desenvolvimento e a adaptação de práticas e materiais instrucionais diversos (e.g., "espelhos" de isopor e "raios luminosos" de bolinhas de gude; montagens envolvendo velas, lasers, lentes e espelhos; desmonte e análise de peças de um telescópio; etc.). Além disto, como outro resultado deste trabalho, elaboramos textos sobre história da astronomia e da óptica para atividades em classe. Com estas ações visamos facilitar a concretização de conceitos físicos envolvidos, exemplificar um ensino contextualizado e interdisciplinar motivado por temas astronômicos e favorecer que práticas e discussões feitas com os treinandos possam ser transpostas para a sala de aula. A reação dos professores às práticas propostas foi bastante positiva. Todos esses aspectos são discutidos em detalhe neste trabalho. (PPGECNM/UFRN; PRONEX/FINEP; NUPA/USP; Temáticos/FAPESP)

  5. Studies of relativistic effects with radioastron space mission

    Directory of Open Access Journals (Sweden)

    Zakharov A.F.

    2007-01-01

    Full Text Available In the review we discuss possible studies of GR phenomena such as gravitational microlensing and shadow analysis with the forthcoming RadioAstron space mission. It is well-known that gravitational lensing is a powerful tool in the investigation of the distribution of matter, including that of dark matter (DM. Typical angular distances between images and typical time scales depend on the gravitational lens masses. For the microlensing, angular distances between images or typical astrometric shifts are about 10-5 – 10-6 as1. Such an angular resolution will be reached with the space-ground VLBI interferometer, Radioastron. The basic targets for microlensing searches should be bright point-like radio sources at cosmological distances. In this case, an analysis of their variability and a reliable determination of microlensing could lead to an estimation of their cosmological mass density. Moreover, one could not exclude the possibility that non-baryonic dark matter could also form microlenses if the corresponding optical depth were high enough. It is known that in gravitationally lensed systems, the probability (the optical depth to observe microlensing is relatively high; therefore, for example, such gravitationally lensed objects, like CLASS gravitational lens B1600+434, appear the most suitable to detect astrometric microlensing, since features of photometric microlensing have been detected in these objects. However, to directly resolve these images and to directly detect the apparent motion of the knots, the Radioastron sensitivity would have to be improved, since the estimated flux density is below the sensitivity threshold, alternatively, they may be observed by increasing the integration time, assuming that a radio source has a typical core - jet structure and microlensing phenomena are caused by the superluminal apparent motions of knots. In the case of a confirmation (or a disproval of claims about microlensing in grav­itational lens

  6. El círculo meridiano automático de San Fernando - San Juan. Sus primeros pasos en el hemisferio sur

    Science.gov (United States)

    Mallamaci, C. C.; Muiños, J. L.; Gallego, M.; Pérez, J. A.; Marmolejo, L.; Navarro, J. L.; Sedeño, J.; Vallejos, M.; Belizón, F.

    Se informa sobre el estado actual del Círculo Meridiano Automático de San Fernando-San Juan. El instrumento (Grubb-Parson, de 178mm de abertura y 2665 mm de distancia focal) es gemelo del que se encuentra en las Islas Canarias, y fue instalado durante los meses de julio y agosto de 1996 en la estación astronómica ``Dr. C.U.Cesco" (El Leoncito, Barreal), a unos 200 km de distancia de la ciudad de San Juan, merced a un Convenio de Cooperación Científica, firmado en 1994 entre el ROA (España) y el OAFA (Argentina). En la actualidad se está llevando a cabo un programa de prueba cuyos resultados preliminares muestran que el telescopio está en buenas condiciones para observar estrellas de hasta magnitud aproximada 14.5, con buenos errores de observación (<0.12" en ascensión recta y declinación).

  7. Exploración del catálogo de objetos en emisión H de Henize y All Sky Automated Survey: nuevas variables y tipos espectrales

    Science.gov (United States)

    Jaque Arancibia, M.; Barbá, R. H.; Collado, A.; Gamen, R.; Arias, J. I.

    2016-08-01

    Large astronomical surveys allow us to do systematic studies of stellar populations with significant statistical weight. In this study, we have cross-correlated the Henize's (1976) catalog of stellar sources with H emission-line with “The All Sky Automated Survey'' database. After the positional cross-matching we have found that 1402 of 1926 H sources have ASAS light-curves. From that number, more than 50 (723 sources) are periodic variables with amplitude larger than 0.05 magnitudes, while 276 sources show photometric variations without a clear periodicity. Variable stars that we have found are of many different types, among them Miras, eclipsing binaries, bursting stars, etc. Also, only 133 stars are known previously as variable sources in ASAS catalogue, and 93 of them were studied previously in detail. In order to characterize the nature of the sources, we have started a medium-resolution spectroscopic survey of the unstudied variable emission-line objects using the 2.15-m Jorge Sahade Telescope at Complejo Astronómico El Leoncito (Argentina). At the moment, we have observed a set of 67 blue stars selected using 2MASS colors, being almost all of them Be-type stars. This set of bright new variable Be-type stars is ideal for follow-up monitoring for the study of the Be-phenomenon.

  8. PIRATE: A Remotely Operable Telescope Facility for Research and Education

    Science.gov (United States)

    Holmes, S.; Kolb, U.; Haswell, C. A.; Burwitz, V.; Lucas, R. J.; Rodriguez, J.; Rolfe, S. M.; Rostron, J.; Barker, J.

    2011-10-01

    We introduce PIRATE, a new remotely operable telescope facility for use in research and education, constructed from off-the-shelf hardware, operated by The Open University. We focus on the PIRATE Mark 1 operational phase, in which PIRATE was equipped with a widely used 0.35 m Schmidt-Cassegrain system (now replaced with a 0.425 m corrected Dall-Kirkham astrograph). Situated at the Observatori Astronòmic de Mallorca, PIRATE is currently used to follow up potential transiting extrasolar planet candidates produced by the SuperWASP North experiment, as well as to hunt for novae in M31 and other nearby galaxies. It is operated by a mixture of commercially available software and proprietary software developed at the Open University. We discuss problems associated with performing precision time-series photometry when using a German Equatorial Mount, investigating the overall performance of such off-the-shelf solutions in both research and teaching applications. We conclude that PIRATE is a cost-effective research facility, and it also provides exciting prospects for undergraduate astronomy. PIRATE has broken new ground in offering practical astronomy education to distance-learning students in their own homes.

  9. The Kinematics of the Permitted C ii λ 6578 Line in a Large Sample of Planetary Nebulae

    Energy Technology Data Exchange (ETDEWEB)

    Richer, Michael G.; Suárez, Genaro; López, José Alberto; García Díaz, María Teresa, E-mail: richer@astrosen.unam.mx, E-mail: gsuarez@astro.unam.mx, E-mail: jal@astrosen.unam.mx, E-mail: tere@astro.unam.mx [Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, Baja California (Mexico)

    2017-03-01

    We present spectroscopic observations of the C ii λ 6578 permitted line for 83 lines of sight in 76 planetary nebulae at high spectral resolution, most of them obtained with the Manchester Echelle Spectrograph on the 2.1 m telescope at the Observatorio Astronómico Nacional on the Sierra San Pedro Mártir. We study the kinematics of the C ii λ 6578 permitted line with respect to other permitted and collisionally excited lines. Statistically, we find that the kinematics of the C ii λ 6578 line are not those expected if this line arises from the recombination of C{sup 2+} ions or the fluorescence of C{sup +} ions in ionization equilibrium in a chemically homogeneous nebular plasma, but instead its kinematics are those appropriate for a volume more internal than expected. The planetary nebulae in this sample have well-defined morphology and are restricted to a limited range in H α line widths (no large values) compared to their counterparts in the Milky Way bulge; both these features could be interpreted as the result of young nebular shells, an inference that is also supported by nebular modeling. Concerning the long-standing discrepancy between chemical abundances inferred from permitted and collisionally excited emission lines in photoionized nebulae, our results imply that multiple plasma components occur commonly in planetary nebulae.

  10. STS-61 crew utilizing Virtual Reality in training for HST repair mission

    Science.gov (United States)

    1993-01-01

    Astronaut Jeffrey A. Hoffman, one of four crewmembers for STS-61 that will conduct scheduled spacewalks during the flight, wears a special helmet and gloves designed to assist in proper positioning near the telescope while on the end of the robot arm. Crewmembers are utilizing a new virtual reality training aid which assists in refining positioning patterns for Space Shuttle Endeavour's Remote Manipulator System (RMS) (36890); Astronaut Claude Nicollier looks at a computer display of the Shuttle's robot arm movements as Thomas D. Akers and Kathryn C. Thornton, mission specialists look on. Nicollier will be responsible for maneuvering the astronauts while they stand in a foot restraint on the end of the RMS arm (36891,36894); Hoffman wears a special helmet and gloves designed to assist in proper positioning near the telescope while on the end of the robot arm (35892); Nicollier looks at a computer display of the Shuttle's robot arm movements as Akers looks on (36893); While (l-r) Astron

  11. Inflationary scenario from higher curvature warped spacetime

    Energy Technology Data Exchange (ETDEWEB)

    Banerjee, Narayan [Indian Institute of Science Education and Research Kolkata, Department of Physical Sciences, Nadia, West Bengal (India); Paul, Tanmoy [Indian Association for the Cultivation of Science, Department of Theoretical Physics, Kolkata (India)

    2017-10-15

    We consider a five dimensional warped spacetime, in presence of the higher curvature term like F(R) = R + αR{sup 2} in the bulk, in the context of the two-brane model. Our universe is identified with the TeV scale brane and emerges as a four dimensional effective theory. From the perspective of this effective theory, we examine the possibility of ''inflationary scenario'' by considering the on-brane metric ansatz as an FRW one. Our results reveal that the higher curvature term in the five dimensional bulk spacetime generates a potential term for the radion field. Due to the presence of radion potential, the very early universe undergoes a stage of accelerated expansion and, moreover, the accelerating period of the universe terminates in a finite time. We also find the spectral index of curvature perturbation (n{sub s}) and the tensor to scalar ratio (r) in the present context, which match with the observational results based on the observations of Planck (Astron. Astrophys. 594, A20, 2016). (orig.)

  12. Gravastars in f (R ,T ) gravity

    Science.gov (United States)

    Das, Amit; Ghosh, Shounak; Guha, B. K.; Das, Swapan; Rahaman, Farook; Ray, Saibal

    2017-06-01

    We propose a unique stellar model under the f (R ,T ) gravity by using the conjecture of Mazur-Mottola [P. Mazur and E. Mottola, Report No. LA-UR-01-5067, P. Mazur and E. Mottola, Proc. Natl. Acad. Sci. USA 101, 9545 (2004), 10.1073/pnas.0402717101] which is known as gravastar and a viable alternative to the black hole as available in literature. This gravastar is described by the three different regions, viz., (I) Interior core region, (II) Intermediate thin shell, and (III) Exterior spherical region. The pressure within the interior region is equal to the constant negative matter density which provides a repulsive force over the thin spherical shell. This thin shell is assumed to be formed by a fluid of ultrarelativistic plasma and the pressure, which is directly proportional to the matter-energy density according to Zel'dovich's conjecture of stiff fluid [Y. B. Zel'dovich, Mon. Not. R. Astron. Soc. 160, 1 (1972), 10.1093/mnras/160.1.1P], does counterbalance the repulsive force exerted by the interior core region. The exterior spherical region is completely vacuum and assumed to be de Sitter spacetime which can be described by the Schwarzschild solution. Under this specification we find out a set of exact and singularity-free solution of the gravastar which presents several other physically valid features within the framework of alternative gravity.

  13. Relativistic dust accretion of charged particles in Kerr-Newman spacetime

    Science.gov (United States)

    Schroven, Kris; Hackmann, Eva; Lämmerzahl, Claus

    2017-09-01

    We describe a new analytical model for the accretion of particles from a rotating and charged spherical shell of dilute collisionless plasma onto a rotating and charged black hole. By assuming a continuous injection of particles at the spherical shell and by treating the black hole and a featureless accretion disk located in the equatorial plane as passive sinks of particles, we build a stationary accretion model. This may then serve as a toy model for plasma feeding an accretion disk around a charged and rotating black hole. Therefore, our new model is a direct generalization of the analytical accretion model introduced by E. Tejeda, P. A. Taylor, and J. C. Miller [Mon. Not. R. Astron. Soc. 429, 925 (2013), 10.1093/mnras/sts316]. We use our generalized model to analyze the influence of a net charge of the black hole, which will in general be very small, on the accretion of plasma. Within the assumptions of our model we demonstrate that already a vanishingly small charge of the black hole may in general still have a non-negligible effect on the motion of the plasma, as long as the electromagnetic field of the plasma is still negligible. Furthermore, we argue that the inner and outer edges of the forming accretion disk strongly depend on the charge of the accreted plasma. The resulting possible configurations of accretion disks are analyzed in detail.

  14. Chilean Astronomers and the Birth of Cerro Tololo

    Science.gov (United States)

    Moreno, H.

    1990-11-01

    P# JMEN. Hace treinta afios que se tnict6 en Chile la de n luga adecuado pata establecer observatoro astron6ini- Co, que a en wi ieflector de 1 in de diam'etrr . importante destacar el papel que le corres-pondi6 al Obseiwatorio Nacional de Ia Universidad de `Chile -- re'.-. tarde Departamento de de la inisma Univer- sidad .- en 1 de este proycoto. Los resultados han ido mucho mct5 impoftaftes lo esperado . de tal nodo q. el prc -ama destinado a instalar ui telescopio de tama- f ha I levado al establ ecimiento de iri centro de acti- cientfica de relieve inten-acional. ALb(TRA . Thifty years ago the search for a site adequate for the est 1ishment of an astronomical was fn (Thile. Initially it was planned that the main telescope would be a 1 in i-cf lector. It is importaft to the role played by th O Astm-'n6mioo Nacional de la Unfversidad de Cbf Ic - later 0: Depaftamento de of the same University - in the development of this project. The results have been much more important than was e:-:pected initially: in thiS way the prr gram for a telescope of moderate size was transfo -med in a major project wh i ch 1 cad to the estab 1 ). shinent of an i nt i ona 1 center of scieftific research. AQ/ W : OBSERVATORIES

  15. Development of a Lunar Scintillometer as part of the national large optical telescope site survey

    Science.gov (United States)

    Surendran, Avinash; Parihar, Padmakar S.; Banyal, Ravinder K.; Kalyaan, Anusha

    2018-01-01

    Ground layer turbulence is a very important site characterization parameter used to assess the quality of an astronomical site. The Lunar Scintillometer is a simple and effective site-testing device for measuring the ground layer turbulence. It consists of a linear array of photodiodes which are sensitive to the slight variations in the moon's brightness due to scintillation by the lower layers of the Earth's atmosphere. The covariance of intensity values between the non-redundant photodiode baselines can be used to measure the turbulence profile from the ground up to a height determined by the furthest pair of detectors. The six channel lunar scintillometer that has been developed at the Indian Institute of Astrophysics is based closely on an instrument built by the team led by Andrei Tokovinin of Cerro Tololo Inter-American Observatory (CTIO), Chile (Tokovinin et al., Mon. Not. R. Astron. Soc. 404(3), 1186-1196 2010). We have fabricated the instrument based on the existing electronic design, and have worked on the noise analysis, an EMI (Electromagnetic Induction) resistant PCB design and the software pipeline for analyzing the data from the same. The results from the instrument's multi-year campaign at Mount Saraswati, Hanle is also presented.

  16. Evaluating the New Automatic Method for the Analysis of Absorption Spectra Using Synthetic Spectra

    Directory of Open Access Journals (Sweden)

    Matthew B. Bainbridge

    2017-04-01

    Full Text Available We recently presented a new “artificial intelligence” method for the analysis of high-resolution absorption spectra (Bainbridge and Webb, Mon. Not. R. Astron. Soc. 2017, doi:10.1093/mnras/stx179. This new method unifies three established numerical methods: a genetic algorithm (GVPFIT; non-linear least-squares optimisation with parameter constraints (VPFIT; and Bayesian Model Averaging (BMA. In this work, we investigate the performance of GVPFIT and BMA over a broad range of velocity structures using synthetic spectra. We found that this new method recovers the velocity structures of the absorption systems and accurately estimates variation in the fine structure constant. Studies such as this one are required to evaluate this new method before it can be applied to the analysis of large sets of absorption spectra. This is the first time that a sample of synthetic spectra has been utilised to investigate the analysis of absorption spectra. Probing the variation of nature’s fundamental constants (such as the fine structure constant, through the analysis of absorption spectra, is one of the most direct ways of testing the universality of physical laws. This “artificial intelligence” method provides a way to avoid the main limiting factor, i.e., human interaction, in the analysis of absorption spectra.

  17. Evolving coma abundances and detection of hypervolatiles in Jupiter-family comet 45P/Honda-Mrkos-Pajdusakova

    Science.gov (United States)

    Dello Russo, Neil; DiSanti, Michael A.; Kawakita, Hideyo; Shinnaka, Yoshiharu; Vervack, Ronald J.; Bonev, Boncho P.; Gibb, Erika L.; Roth, Nathan; McKay, Adam J.; Weaver, Harold A.; Cochran, Anita L.

    2017-10-01

    Two major shortcomings in chemically classifying comets at infrared wavelengths are a lack of hypervolatile (CO and CH4) detections in Jupiter-family comets and incomplete temporal coverage of comet chemistry, particularly at small heliocentric distances (Rh). We report post-perihelion volatile abundances in comet 45P/Honda-Mrkos-Pajdusakova with the high-resolution infrared spectrometer iSHELL at the NASA/IRTF on UT 6 - 8 January when Rh = 0.55 AU (DiSanti et al. 2017, Astron. J., in press), and with NIRSPEC at the Keck Observatory on UT 13 and 19 February when Rh = 1.0 and 1.1 AU, respectively. Favorable comet geocentric velocities enabled the detection of CO and CH4 in early January and 19 February. The relative abundance of CO is severely depleted whereas CH4 is typical to enriched in 45P when compared to comets from the Oort cloud. Significant differences are seen in relative abundances of species between January and February, notably in the ratio of C2H2/HCN. We explore whether the heliocentric distances of the measurements or seasonal changes primarily cause these differences by comparing to observations of C/2012 S1 ISON obtained over a similar range of heliocentric distances. NASA and NSF research grants support this work. We also acknowledge the expert support of the IRTF and Keck support staffs during these observations.

  18. Conversations with Marcgrave: the Origin of Modern Astronomy in the Southern Hemisphere (Spanish Title: Conversando con Marcgrave: El Origen de la Astronomía Moderna en el Hemisferio Sur) Conversando Com Marcgrave: a Origem da Moderna Astronomia no Hemisfério Sul

    Science.gov (United States)

    Medeiros, Alexandre; Araújo, Fábio

    2005-12-01

    primer observatorio astronómico del hemisferio y autor de las primeras observaciones astronómicas sistemáticas utilizando telescopios de este lado del mundo. Nuestra "conversación" con Marcgrave es imaginada en el marco del Recife antiguo, lugar donde él vivió durante el período de Mauricio de Nassau, y reune algunos colegas profesores apasionados por la enseñanza de la Astronomía. La historia es contada, de esta forma, dentro de un clima ameno y hasta un poco divertido, si bien las informaciones históricas y conceptuales contenidas en ella están basadas en fuentes bibliográficas confiables, debidamente referenciadas al final del texto. Estas fuentes van desde la obra original de este científico, en la cual aparece su relato sobre la observación de un eclipse solar en Recife, pasando por obras clásicas respecto de él mismo, como la del profesor Juliano Moreira, hasta fuentes mucho más recientes como el influyente trabajo del profesor John North. Otros textos importantes referidos al período de la colonización holandesa en el Brasil, tales como las obras clásicas de Charles Boxer, Bouman y Boogaart entre otros, son también utilizados en la construcción de esta dramatización pedagógica que se refiere a un interesante capítulo de la Historia de la Astronomía. O ano de 2004 assinala os 400 anos do nascimento do conde Maurício de Nassau, um importante personagem da história do Brasil. O presente texto está relacionado com o período do domínio holandês em Pernambuco. O artigo tenta resgatar o começo do estudo da Astronomia no hemisfério Sul. Para tal, idealizamos uma dramatização de uma entrevista fictícia com o astrônomo alemão Georg Marcgrave, construtor do primeiro observatório astronômico deste hemisfério e autor das primeiras observações astronômicas sistemáticas com o uso de telescópios neste lado do mundo. Nossa "conversa" com Marcgrave é idealizada no cenário do Recife antigo, local em que ele viveu no período de Maur

  19. Ozone exposure of field-grown winter wheat affects soil mesofauna in the rhizosphere

    Energy Technology Data Exchange (ETDEWEB)

    Schrader, Stefan, E-mail: stefan.schrader@vti.bund.d [Johann Heinrich von Thuenen-Institute (vTI), Federal Research Institute for Rural Areas, Forestry and Fisheries, Institute of Biodiversity, Bundesallee 50, 38116 Braunschweig (Germany); Bender, Juergen; Weigel, Hans-Joachim [Johann Heinrich von Thuenen-Institute (vTI), Federal Research Institute for Rural Areas, Forestry and Fisheries, Institute of Biodiversity, Bundesallee 50, 38116 Braunschweig (Germany)

    2009-12-15

    A 2-year open-top chamber experiment with field-grown winter wheat (Triticum aestivum L. cv. Astron) was conducted to examine the effects of ozone on plant growth and selected groups of soil mesofauna in the rhizosphere. From May through June in each year, plants were exposed to two levels of O{sub 3}: non-filtered (NF) ambient air or NF+ 40 ppb O{sub 3} (NF+). During O{sub 3} exposure, soil sampling was performed at two dates according to different plant growth stages. O{sub 3} exposure reduced above- and below-ground plant biomass in the first year, but had little effect in the second year. The individual density of enchytraeids, collembolans and soil mites decreased significantly in the rhizosphere of plants exposed to NF+ in both years. Differences were highest around anthesis, i.e. when plants are physiologically most active. The results suggest that elevated O{sub 3} concentrations may influence the dynamic of decomposition processes and the turnover of nutrients. - Ozone reduced the individual densities of enchytraeids, collembolans and soil mites in the rhizosphere of winter wheat indirectly via the plant-soil-system.

  20. La astronomía de un humanista, Juan Andrés

    Directory of Open Access Journals (Sweden)

    José Antonio SANDUVETE CHAVES

    2009-11-01

    Full Text Available RESUMEN: La páginas que siguen pretenden ofrecer una visión de conjunto del análisis que de la historia de la Astronomía realiza Juan Andrés, desde los orígenes de la humanidad hasta el siglo XVIII. Este análisis, incluido en su monumental obra Origen, progresos y estado actual de toda la literatura, destaca por su modernidad y precisión, constituyendo, por tanto, una interesante base de comparación entre la visión de la ciencia astronómica del humanismo ilustrado y la que pervive en la actualidad.ABSTRACT: The following pages attempt to offer a full view of the research into the history of astronomy made by Juan Andrés, from the beginning of human culture until the 18th century. This analysis, included in a broader work called Origen, progresos y estado de toda la literatura, stands out on account of its modern and precise ideas, thus representing an interesting knowledge base for comparing the view of astronomy during the Enlightenment with that of the present.

  1. La regeneración de la astronomía y la meteorología españolas: Augusto Arcimís (1844-1910 y el institucionismo

    Directory of Open Access Journals (Sweden)

    Anduaga Egaña, Aitor

    2005-12-01

    Full Text Available The article is about the attempts for regenerating Spanish astronomy and meteorology in the last quarter of the twentieth century through the human and scientific trajectory of Augusto Arcimís (1844-1910, amateur astronomer and the first Spanish professional meteorologist. The role of personalities linked to the Institución Libre de Enseñanza in the creation of the Instituto Central Meteorológico in 1887 and the spread of modern astronomical theories is analyzed.

    El artículo trata sobre los intentos por regenerar la astronomía y la meteorología españolas durante el último cuarto del siglo XIX a través de la trayectoria científica y humana del astrónomo amateur y primer meteorólogo profesional español Augusto Arcimís (1844-1910. Se estudia el papel de personalidades vinculadas a la Institución Libre de Enseñanza en la creación del Instituto Central Meteorológico en 1887 y en la difusión de teorías astronómicas modernas.

  2. Secular resonances between bodies on close orbits II: prograde and retrograde orbits for irregular satellites

    Science.gov (United States)

    Li, Daohai; Christou, Apostolos A.

    2017-09-01

    In extending the analysis of the four secular resonances between close orbits in Li and Christou (Celest Mech Dyn Astron 125:133-160, 2016) (Paper I), we generalise the semianalytical model so that it applies to both prograde and retrograde orbits with a one-to-one map between the resonances in the two regimes. We propose the general form of the critical angle to be a linear combination of apsidal and nodal differences between the two orbits b_1 Δ π + b_2 Δ Ω, forming a collection of secular resonances in which the ones studied in Paper I are among the strongest. Test of the model in the orbital vicinity of massive satellites with physical and orbital parameters similar to those of the irregular satellites Himalia at Jupiter and Phoebe at Saturn shows that {>}20 and {>}40% of phase space is affected by these resonances, respectively. The survivability of the resonances is confirmed using numerical integration of the full Newtonian equations of motion. We observe that the lowest order resonances with b_1+|b_2|≤ 3 persist, while even higher-order resonances, up to b_1+|b_2|≥ 7, survive. Depending on the mass, between 10 and 60% of the integrated test particles are captured in these secular resonances, in agreement with the phase space analysis in the semianalytical model.

  3. Programas de aplicación de agrometeorología para docencia e investigación

    Directory of Open Access Journals (Sweden)

    Bombelli, Enrique

    2009-01-01

    Full Text Available Para el estudio de las Ciencias Meteorológicas y Climáticas aplicadas al agro, es necesario estimar procesos matemáticos y físicos para interpretar la interacción de los procesos atmosféricos y biológicos, los cuales se pueden automatizar haciendo énfasis en el análisis de los mismos. El presente trabajo tiene como objetivo mostrar las características de un software de aplicación utilizado para en la enseñanza de la Climatología Agrícola, que estima parámetros tales como: Radiación Astronómica y Global, diferentes metodologías de cálculo de la Evapotranspiración Potencial y el Balance Hidrológico Climático entre otros. El software Programas de aplicación de Agroclimatología, realizado en la Facultad de Agronomía de la Universidad de Buenos Aires, brinda al alumno un rápido manejo de resultados, con la posibilidad de realizar interpretaciones de distintas variables para diferentes localidades, de manera de poder visualizar y analizar los resultados que surgen de las distintas corridas.

  4. Fast numerics for the spin orbit equation with realistic tidal dissipation and constant eccentricity

    Science.gov (United States)

    Bartuccelli, Michele; Deane, Jonathan; Gentile, Guido

    2017-08-01

    We present an algorithm for the rapid numerical integration of a time-periodic ODE with a small dissipation term that is C^1 in the velocity. Such an ODE arises as a model of spin-orbit coupling in a star/planet system, and the motivation for devising a fast algorithm for its solution comes from the desire to estimate probability of capture in various solutions, via Monte Carlo simulation: the integration times are very long, since we are interested in phenomena occurring on timescales of the order of 10^6-10^7 years. The proposed algorithm is based on the high-order Euler method which was described in Bartuccelli et al. (Celest Mech Dyn Astron 121(3):233-260, 2015), and it requires computer algebra to set up the code for its implementation. The payoff is an overall increase in speed by a factor of about 7.5 compared to standard numerical methods. Means for accelerating the purely numerical computation are also discussed.

  5. Morfología de la Coma del Cometa Hale - Bopp

    Science.gov (United States)

    Gil-Hutton, R.; Caballero, M.; Coldwell, G.; Cañada, M.; Godoy, G.; Trozzo, C.; Gómez, G.

    Para lograr comprender plenamente los procesos físicos que se desarrollan en los núcleos cometarios y obtener un modelo que explique, no sólo su actividad, sino también sus efectos sobre la coma, es necesario obtener información detallada para el mayor número de cometas posible, siendo las características más interesantes para estudiar la ubicación de las regiones activas, la presencia de jets, las tasas de producción de gas y polvo y la interacción de la coma con el viento solar. En la actualidad, con técnicas de procesamiento de imágenes y tecnología CCD se pueden obtener este tipo de datos para cometas que ingresan al sistema solar interior y estudiar, de esta manera, la morfología de sus comas, tratando de correlacionar la actividad detectada con algún modelo teórico. En este trabajo se presenta un estudio parcial de la actividad desarrollada por el cometa Hale-Bopp, y sus efectos sobre la morfología de su coma, desde agosto de 1995 hasta la fecha en base a imágenes adquiridas con el telescopio de 0.76 m. de la Estación Astronómica Dr. Carlos Ulrrico Cesco.

  6. On the HCN – HNC Energy Difference

    Energy Technology Data Exchange (ETDEWEB)

    Nguyen, Thanh L.; Baraban, Joshua H.; Ruscic, Branko; Stanton, John F.

    2015-11-05

    The value for the HCN → HNC 0 K isomerization energy has been investigated by combining state-of-the-art electronic structure methods with the Active Thermochemical Tables (ATcT) approach. The directly computed energy difference between HCN and HNC at the HEAT-456QP level of theory is 5236 ± 50 cm–1. This is substantially lower (by ~470 cm–1 or ~1.3 kcal/mol) than the recently proposed high-level multireference configuration interaction value of 5705 ± 20 cm–1 of Barber et al. (Mon. Not. R. Astron. Soc.2014, 437, 1828–1835). The discrepancy was analyzed by the ATcT approach, using several distinct steps, which (a) independently corroborated the current single-reference HEAT-456QP result, (b) independently found that the recent multireference-based value is highly unlikely to be correct within its originally stated uncertainty, and (c) produced a recommended value of 5212 ± 30 cm–1 for the HCN → HNC isomerization energy at 0 K, based on all currently available knowledge. The ATcT standard enthalpies of formation at 0 and 298 K for HCN, HNC, and their cations and anions are also presented.

  7. On the shear instability in relativistic neutron stars

    Energy Technology Data Exchange (ETDEWEB)

    Corvino, Giovanni; Rezzolla, Luciano; Giacomazzo, Bruno [Max-Planck-Institut fuer Gravitationsphysik, Albert-Einstein-Institut, Golm (Germany); Bernuzzi, Sebastiano [Theoretical Physics Institute, University of Jena, 07743 Jena (Germany); De Pietri, Roberto, E-mail: Giovanni.Corvino@roma1.infn.i [Physics Department, Parma University and INFN, Parma (Italy)

    2010-06-07

    We present new results on instabilities in rapidly and differentially rotating neutron stars. We model the stars in full general relativity and describe the stellar matter adopting a cold realistic equation of state based on the unified SLy prescription (Douchin and Haensel 2001 Astron. Astrophys. 380 151-67). We provide evidence that rapidly and differentially rotating stars that are below the expected threshold for the dynamical bar-mode instability, {beta}{sub c} {identical_to} T/|W| {approx_equal} 0.25, do nevertheless develop a shear instability on a dynamical timescale and for a wide range of values of {beta}. This class of instability, which has so far been found only for small values of {beta} and with very small growth rates, is therefore more generic than previously found and potentially more effective in producing strong sources of gravitational waves. Overall, our findings support the phenomenological predictions made by Watts et al (2005 Astrophys. J. 618 L37) on the nature of the low-T/|W| instability as the manifestation of a shear instability in a region where the latter is possible only for small values of {beta}. Furthermore, our results provide additional insight on shear instabilities and on the necessary conditions for their development.

  8. Foco Nasmyth para el telescopio 2,15mts. de CASLEO

    Science.gov (United States)

    Casagrande, A. R.

    En principio, este proyecto intenta lograr el mayor aprovechamiento posible del instrumental que se dispone, buscando la manera de optimizar y hacer más eficiente el servicio que brinda el CASLEO a la comunidad astronómica. El mismo consiste en utilizar dispositivos ya existentes en el telescopio, y darle una utilidad. Tal es el caso del camino óptico destinado al foco Coude. Si tenemos en cuenta que disponemos de un tercer espejo Coude, con todos sus mecanismos automatizados, (actualmente sin uso), una distancia apropiada del plano focal, el espacio y el lugar físico necesario para instalar un periférico, es posible la habilitación de un foco Nasmyth en el telescopio 2,15mts. El hecho de contar con este nuevo foco, redundará en importantes beneficios. En primer lugar, posibilitará la observación, casi simultánea, con dos instrumentos. Otro aspecto a tener en cuenta, es que disminuirá el frecuente cambio del instrumental periférico, motivo este que degrada su ideal puesta a punto. Por último, también de interés, es de destacar su escaso costo de ejecución.

  9. A unifying fractional wave equation for compressional and shear waves.

    Science.gov (United States)

    Holm, Sverre; Sinkus, Ralph

    2010-01-01

    This study has been motivated by the observed difference in the range of the power-law attenuation exponent for compressional and shear waves. Usually compressional attenuation increases with frequency to a power between 1 and 2, while shear wave attenuation often is described with powers less than 1. Another motivation is the apparent lack of partial differential equations with desirable properties such as causality that describe such wave propagation. Starting with a constitutive equation which is a generalized Hooke's law with a loss term containing a fractional derivative, one can derive a causal fractional wave equation previously given by Caputo [Geophys J. R. Astron. Soc. 13, 529-539 (1967)] and Wismer [J. Acoust. Soc. Am. 120, 3493-3502 (2006)]. In the low omegatau (low-frequency) case, this equation has an attenuation with a power-law in the range from 1 to 2. This is consistent with, e.g., attenuation in tissue. In the often neglected high omegatau (high-frequency) case, it describes attenuation with a power-law between 0 and 1, consistent with what is observed in, e.g., dynamic elastography. Thus a unifying wave equation derived properly from constitutive equations can describe both cases.

  10. Alcune osservazioni sulle occorenze di Crux in Manilio, Séneca, Giovenale, Marziale

    Directory of Open Access Journals (Sweden)

    Ilaria Ramelli

    1999-01-01

    Full Text Available II supplizio della croce appare un tema particolarmente presente e diffuso nella letteratura latina del i secólo d.C. Manilio, nel V libro del suoi Astronómica, per la prima voita attñbuisce la croce ad Andrómeda, operando una vistosa innovazione all'interno della tradizione mitografica. Ma anche Petronio, tucano. Séneca, Giovenale e Marziale parlano piú volte della croce. Séneca ne appare Impresslonato in modo speclale e Marziale cita il caso di uno schiavo crocifisso per avere Incendiato Roma. Cosi Giovenale sembra fare allusione ai supplizl inflitti ai Cristiani con l'accusa di avere incendiato Roma (64 d.C..The torment of the cross is a theme that Is partlcularly present in the Román literatura of the ist century A.D. Manilius for the first time ascrlbes the cross to Andrómeda, with a remarkable innovation in the mythographic tradition. But also Petronius, Lucan, Séneca, Juvenai and Martial In several occasions mention the cross. Séneca appears particuiariy impressed by this torment. Martial represents a slave hanging from the cross as guilty of the fire of Rome. And so Juvenai seems to allude to the torments infiicted to the Christians as scapegoats of the fire of Rome (64 A.D..

  11. Anisotropic compact star models in Karmarkar space time continuum

    Science.gov (United States)

    Fuloria, Pratibha

    2017-12-01

    In the present article, we have explored some new anisotropic compact star models by using embedded class one space time metric. We proceed our calculations by assuming a particular form of g_{rr} metric potential and solved for the other metric g_{tt} using Karmarkar condition. The matter density, radial pressure, tangential pressure, mass function, surface red-shift, anisotropy are all well behaved inside the fluid sphere. The solution satisfies all energy conditions i.e. strong energy condition, null energy condition, dominant energy condition and weak energy condition. The solution also satisfies the causality condition and can represent stable stellar fluid system as the adiabatic index Γ > 4/3 and the stability factor -1≤ vt2-vr2≤ 0 holds good inside the fluid sphere. We have framed our solution for two compact stars PSR J1614-2230 and SAX J1808.4-3658, which are well-behaved in all respects. The mass and radius of the compact stars PSR J1614-2230 and SAXJ1808.4-3658, obtained from the models are very close to the observational data proposed by Gangopadhyay et al. (Mon. Not. R. Astron. Soc. 431:3216, 2013) and Bhattacharya (2001) respectively.

  12. Cosmology with Minkowski functionals and moments of the weak lensing convergence field

    Science.gov (United States)

    Petri, Andrea; Haiman, Zoltán; Hui, Lam; May, Morgan; Kratochvil, Jan M.

    2013-12-01

    We compare the efficiency of moments and Minkowski functionals (MFs) in constraining the subset of cosmological parameters (Ωm,w,σ8) using simulated weak lensing convergence maps. We study an analytic perturbative expansion of the MFs [T. Matsubara, Phys. Rev. D 81, 083505 (2010); D. Munshi et al., Mon. Not. R. Astron. Soc. 419, 536 (2012)] in terms of the moments of the convergence field and of its spatial derivatives. We show that this perturbation series breaks down on smoothing scales below 5', while it shows a good degree of convergence on larger scales (˜15'). Most of the cosmological distinguishing power is lost when the maps are smoothed on these larger scales. We also show that, on scales comparable to 1', where the perturbation series does not converge, cosmological constraints obtained from the MFs are approximately 1.5-2 times better than the ones obtained from the first few moments of the convergence distribution—provided that the latter include spatial information, either from moments of gradients or by combining multiple smoothing scales. Including a set of either these moments or the MFs can significantly tighten constraints on cosmological parameters, compared to the conventional method of using the power spectrum alone.

  13. Impactos ambientais e sociais da Copa do Mundo de 2014 http://dx.doi.org/10.15601/1983-7631/rt.v7n12p59-66

    Directory of Open Access Journals (Sweden)

    Marilia Carla de Mello Gaia

    2014-05-01

    Full Text Available Desde a escolha do Brasil, em 2007, para sediar a Copa do Mundo de Futebol de 2014 e as Olimpíadas de 2016, este é um tema recorrente na mídia e em demais espaços de socialização dos brasileiros. Muitas discussões a cerca destes megaeventos esportivos envolvem os benefícios relacionados ao incentivo ao esporte nacional, ao incremento no turismo e na economia e às obras de infraestrutura (sistema de transporte urbano, aeroportos, arenas esportivas, comércio, etc.. A partir das manifestações populares em junho de 2013, principalmente, amplia-se em uma parcela da população brasileira um outro olhar sobre estes eventos esportivos, sobretudo os questionamentos relacionados às necessidades sociais da população em detrimento dos astronômicos investimentos financeiros e políticos para a Copa. Neste contexto, este artigo se destina a discutir alguns elementos envolvidos nos impactos sociais e ambientais da realização da Copa do Mundo de Futebol e das Olimpíadas no Brasil.

  14. Impactos ambientais e sociais da Copa do Mundo de 2014

    Directory of Open Access Journals (Sweden)

    Marilia Carla de Mello Gaia

    2014-05-01

    Full Text Available Desde a escolha do Brasil, em 2007, para sediar a Copa do Mundo de Futebol de 2014 e as Olimpíadas de 2016, este é um tema recorrente na mídia e em demais espaços de socialização dos brasileiros. Muitas discussões a cerca destes megaeventos esportivos envolvem os benefícios relacionados ao incentivo ao esporte nacional, ao incremento no turismo e na economia e às obras de infraestrutura (sistema de transporte urbano, aeroportos, arenas esportivas, comércio, etc.. A partir das manifestações populares em junho de 2013, principalmente, amplia-se em uma parcela da população brasileira um outro olhar sobre estes eventos esportivos, sobretudo os questionamentos relacionados às necessidades sociais da população em detrimento dos astronômicos investimentos financeiros e políticos para a Copa. Neste contexto, este artigo se destina a discutir alguns elementos envolvidos nos impactos sociais e ambientais da realização da Copa do Mundo de Futebol e das Olimpíadas no Brasil.

  15. Simulación de la trayectoria de un cohete de dos etapas para posicionamiento de un nanosatélite en órbita

    Directory of Open Access Journals (Sweden)

    Jhonathan Orlando Murcia Piñeros

    2014-01-01

    Full Text Available En el presente artículo se estudia el posible lanzamiento de un cohete de dos etapas impulsado por propelentes líquidos tipo RP-1 para transportar una carga útil de 4 kg equivalente a la masa de un nano-satélite de tres unidades de Cubesat. Se plantea el estudio con el diseño conceptual del cohete portador implementando un código computacional de optimización con la finalidad de reducir la masa al despegue y aumentar la velocidad. Se eligió como sitio de lanzamiento desde Colombia a la base del Grupo Aéreo del Oriente (GAORI en Marandúa, Vichada, dado que en la actualidad se realizan investigaciones en lanzamiento de cohetes y ha sido utilizado por universidades para el desarrollo de tales investigaciones. Los valores obtenidos anteriormente son introducidos en un código computacional en FORTRAN desarrollado en el Observatorio Astronómico de la Universidad Nacional de Colombia para obtener el comportamiento de la trayectoria de vuelo del cohete durante su fase de ascenso e inyección orbital.

  16. Successful model for cooperative student learning centers in physics and astronomy

    Science.gov (United States)

    Bieniek, Ronald J.; Johnson, John A.

    2003-04-01

    We have established successful problem-based learning centers for introductory courses in physics [1] and astronomy [2] that fully implement the Seven Principles of Good Practice in Undergraduate Education [3] without increased demand on faculty time. Large percentages of students at our two institutions voluntarily utilize these learning venues. Course instructors guide self-forming groups of students to mastery of technical concepts and skills, building greater student self-confidence through direct interaction and feedback. The approach's immediacy helps students recognize ambiguities in their understanding, thereby increasing impact at teachable moments. Underperforming students are assisted along side students who wish to hone their skills. The format also facilitates racial and gender mixing within learning center camaraderie. Specific pedagogical and operational techniques for running learning centers will be presented. [1] http://www.umr.edu/ physics/plc [2] http://astron.berkeley.edu/talc.html [3] A.W. Chickering & Z.F. Gamson, Am. Assoc. Higher Ed. Bulletin, 1987, 39(7) 3-7.

  17. Long-Term Stability of Planets in the Alpha Centauri System

    Science.gov (United States)

    Lissauer, Jack; Quarles, Billy

    2015-01-01

    The alpha Centauri system is billions of years old, so planets are only expected to be found in regions where their orbits are long-lived. We evaluate the extent of the regions within the alpha Centauri AB star system where small planets are able to orbit for billion-year timescales, and we map the positions in the sky plane where planets on stable orbits about either stellar component may appear. We confirm the qualitative results of Wiegert & Holman (Astron. J. 113, 1445, 1997) regarding the approximate size of the regions of stable orbits of a single planet, which are larger for retrograde orbits relative to the binary than for pro-grade orbits. Additionally, we find that mean motion resonances with the binary orbit leave an imprint on the limits of orbital stability, and the effects of the Lidov-Kozai mechanism are also readily apparent. Overall, orbits of a single planet in the habitable zones near the plane of the binary are stable, whereas high-inclination orbits are short-lived. However, even well within regions where single planets are stable, multiple planet systems must be significantly more widely-spaced than they need to be around an isolated star in order to be long-lived.

  18. Mapping the Region in the Nearest Star System to Search for Habitable Planets

    Science.gov (United States)

    Lissauer, Jack J.; Quarles, B.

    2015-01-01

    Circumstellar planets within the alpha Centauri AB star system have been suggested through formation models and recent observations, and ACESat (Belikov et al. AAS Meeting #225, #311.01, 2015) is a proposed space mission designed to directly image Earth-sized planets in the habitable zones of both of these stars. The alpha Centauri system is billions of years old, so planets are only expected to be found in regions where their orbits are long-lived. We evaluate the extent of the regions within the alpha Centauri AB star system where small planets are able to orbit for billion-year timescales and we map the positions in the sky plane where planets on stable orbits about either stellar component may appear. We confirm the qualitative results of Wiegert & Holman (Astron. J. 113, 1445, 1997) regarding the approximate size of the regions of stable orbits, which are larger for retrograde orbits relative to the binary than for prograde orbits. Additionally, we find that mean motion resonances with the binary orbit leave an imprint on the limits of orbital stability, and the effects of the Lidov-Kozai mechanism are also readily apparent. Overall, orbits in the habitable zones near the plane of the binary are stable, whereas high-inclination orbits are short-lived.

  19. De la astroarqueología a la astronomía cultural

    Directory of Open Access Journals (Sweden)

    Iwaniszewski, Stanislaw

    1994-12-01

    Full Text Available The author outlines a sketch of the development of the study of astronomical and calendrical practices in its sociocultural context during the last thirty years. This study has gone through many changes and these stages may be symbolized by the names of astroarchaeology, megalithic astronomy, archaeoastronomy, ethnoastronomy and cultural astronomy. The author describes this evolution, and the present state of this discipline and then gives a bibliography on the subject in order to promote such research in Spain.

    El autor bosqueja las relaciones entre el estudio de las prácticas calendáricas y astronómicas y el contexto sociocultural al que corresponden durante los últimos treinta años. Los diversos cambios experimentados pueden simbolizarse en los nombres de la astroarqueología. la astronomía megalítica, la arqueoastronomía. la etnoastronomía y la astronomía cultural. El autor describe, además, el estado actual de esta disciplina y proporciona una amplia bibliografía sobre el tema con fines de promover la investigación en España.

  20. Status of the Transneptunian Automated Occultation Survey (TAOS II)

    Science.gov (United States)

    Lehner, Matthew; Wang, Shiang-Yu; Reyes-Ruiz, Mauricio; Alcock, Charles; Castro Chacón, Joel; Chen, Wen-Ping; Chu, You-Hua; Cook, Kem H.; Figueroa, Liliana; Geary, John C.; Hernandez, Benjamin; Huang, Chung-Kai; Norton, Timothy; Szentgyorgyi, Andrew; Yen, Wei-Ling; Zhang, Zhi-Wei

    2017-10-01

    The Transneptunian Automated Occultation Survey (TAOS II) will aim to detect occultations of stars by small (~1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare (<0.001 events per star per year) and short in duration (~200 ms), so many stars must be monitored at a high readout cadence. TAOS II will operate three 1.3 meter telescopes at the Observatorio Astronómico Nacional at San Pedro Mártir in Baja California, México. With a 2.3 square degree field of view and a high speed camera comprising CMOS imagers, the survey will monitor 10,000 stars simultaneously with all three telescopes at a readout cadence of 20 Hz. Construction of the site began in the fall of 2013 and was completed this summer. Telescope installation began in August 2017. This poster will provide an update on the status of the survey development and the schedule leading to the beginning of survey operations.

  1. Russian Space Probes Scientific Discoveries and Future Missions

    CERN Document Server

    Harvey, Brian

    2011-01-01

    The Soviet Union began the exploration of space with the launch of Sputnik in 1957, well over 50 years ago, and sent the first probes to the Moon, Mars, and Venus. Less well known is what these probes actually found out. What were the discoveries of Russian space science? What new discoveries may we expect in the future? Who were Russia's most important scientists? Russian Space Probes gives for the first time the definitive history of Soviet-Russian space science, and is the first book to assess the actual achievements of the Russian space program in furthering our knowledge of the Solar System. Among other projects covered are missions such as Elektron, which mapped the Earth's radiation belts; the astrophysical observatories Astron, Kvant, Gamma, and Granat; Proton, which trapped cosmic rays; Prognoz, which measured solar radiation; and the Interball, Aktivny, APEX, and Magion mission in which satellites chased each other in the Earth's magnetic tail. The final part of the book examines the future of Russ...

  2. Fractal Dimensions of Umbral and Penumbral Regions of Sunspots

    Science.gov (United States)

    Rajkumar, B.; Haque, S.; Hrudey, W.

    2017-11-01

    The images of sunspots in 16 active regions taken at the University College of the Cayman Islands (UCCI) Observatory on Grand Cayman during June-November 2015 were used to determine their fractal dimensions using the perimeter-area method for the umbral and the penumbral region. Scale-free fractal dimensions of 2.09 ±0.42 and 1.72 ±0.4 were found, respectively. This value was higher than the value determined by Chumak and Chumak ( Astron. Astrophys. Trans. 10, 329, 1996), who used a similar method, but only for the penumbral region of their sample set. The umbral and penumbral fractal dimensions for the specific sunspots are positively correlated with r = 0.58. Furthermore, a similar time-series analysis was performed on eight images of AR 12403, from 21 August 2015 to 28 August 2015 taken from the Debrecen Photoheliographic Data (DPD). The correlation is r = 0.623 between the umbral and penumbral fractal dimensions in the time series, indicating that the complexity in morphology indicated by the fractal dimension between the umbra and penumbra followed each other in time as well.

  3. Ten years of SLR production in Argentina

    Science.gov (United States)

    Pacheco, A.; Podestá, R.; Yin, Z.; Liu, W.; Actis, E.; Adarvez, S.; Quinteros, J.; Podestá, F.

    2017-07-01

    SLR technique is a proved astro-geodetic art with a significant power to contribute to Earth and Space Sciences. Therefore, scientific applications of SLR System are able to perform multiple tasks in the fields of Astrometry, Geodesy and Geophysics. The results we show here were obtained from satellite observations made at SLR 7406 Station of Observatorio Astronómico Félix Aguilar (OAFA) in San Juan, Argentina. The telescope was installed early on 2006, in concordance with an International Cooperation Agreement between Universidad Nacional de San Juan, Argentina and Chinese Academy of Sciences. In this abstract we show the current research being done with ILRS 7406 station: Length of day (LOD) and Angular velocity of Earth Rotation, calculated weekly; Pole Motion. ILRS7406 is daily surveying Pole coordinates x and y; Tracking SLR to GNSS constellations. SLR System contributes to the adjustment and validation of satellite GALILEO, GPS, GLONASS, and BEIDOU orbits. Our station is nowadays member of the new ITRF 2014 frame, and these past years has been one of the 3 highest producing SLR Stations on the ILRS net, composed of about 40 stations distributed all around the world. The obtained results during this first 10 years of experience are useful to enhance the traditional collaboration between OAFA and international services such as ILRS, IERS and NASA.

  4. Secular Increase of the Astronomical Unit: a Possible Explanation in Terms of the Total Angular-Momentum Conservation Law

    Science.gov (United States)

    Miura, Takaho; Arakida, Hideyoshi; Kasai, Masumi; Kuramata, Shuichi

    2009-12-01

    We give an idea and order-of-magnitude estimations to explain a recently reported secular increase of the Astronomical Unit (AU) by Krasinsky and Brumberg (Krasinsky & Brumberg 2004, Celest. Mech. Dyn. Astron., 90, 267). The idea proposed is analogous to tidal acceleration in the Earth-Moon system, which is based on conservation of the total angular momentum; we apply this scenario to the Sun-planets system. Assuming the existence of some tidal interactions that transfer the rotational angular momentum of the Sun, and using a reported value of the positive secular trend in the Astronomical Unit, frac{d}{dt}AU = 15±4 (m cy-1), the suggested change in the period of rotation of the Sun is about 21 ms cy-1 in the case that the orbits of the eight planets have the same ``expansion rate.'' This value is sufficiently small, and at present it seems there are no observational data that exclude this possibility. The effects of a change in the Sun's moment of inertia is also investigated. It is pointed out that a change in the moment of inertia due to radiative mass loss by the Sun may be responsible for the secular increase of AU, if orbital ``expansion'' is happening only in the inner-planets system. Although the existence of some tidal interactions is assumed between the Sun and the planets, concrete mechanisms of angular-momentum transfer are not discussed in this paper, which remain to be pursued as future investigations.

  5. Relativistic viscous hydrodynamics for heavy-ion collisions with ECHO-QGP

    Science.gov (United States)

    Del Zanna, L.; Chandra, V.; Inghirami, G.; Rolando, V.; Beraudo, A.; De Pace, A.; Pagliara, G.; Drago, A.; Becattini, F.

    2013-08-01

    We present ECHO-QGP, a numerical code for (3+1)-dimensional relativistic viscous hydrodynamics designed for the modeling of the space-time evolution of the matter created in high-energy nuclear collisions. The code has been built on top of the Eulerian Conservative High-Order astrophysical code for general relativistic magneto-hydrodynamics (Del Zanna et al. in Astron. Astrophys. 473:11, 2007] and here it has been upgraded to handle the physics of the Quark-Gluon Plasma. ECHO-QGP features second-order treatment of causal relativistic viscosity effects both in Minkowskian and in Bjorken coordinates; partial or complete chemical equilibrium of hadronic species before kinetic freeze-out; initial conditions based on the Glauber model, including a Monte-Carlo routine for event-by-event fluctuating initial conditions; a freeze-out procedure based on the Cooper-Frye prescription. The code is extensively validated against several test problems and results always appear accurate, as guaranteed by the combination of the conservative (shock-capturing) approach and the high-order methods employed. ECHO-QGP can be extended to include evolution of the electromagnetic fields coupled to the plasma.

  6. Global positioning system theory and practice

    CERN Document Server

    Hofmann-Wellenhof, Bernhard; Collins, James

    2001-01-01

    This book is dedicated to Dr. Benjamin William Remondi for many reasons. The project of writing a Global Positioning System (GPS) book was con­ ceived in April 1988 at a GPS meeting in Darmstadt, Germany. Dr. Remondi discussed with me the need for an additional GPS textbook and suggested a possible joint effort. In 1989, I was willing to commit myself to such a project. Unfortunately, the timing was less than ideal for Dr. Remondi. Therefore, I decided to start the project with other coauthors. Dr. Remondi agreed and indicated his willingness to be a reviewer. I selected Dr. Herbert Lichtenegger, my colleague from the Technical University Graz, Austria, and Dr. James Collins from Rockville, Maryland, U.S.A. In my opinion, the knowledge ofthe three authors should cover the wide spectrum of GPS. Dr. Lichtenegger is a geodesist with broad experience in both theory and practice. He has specialized his research to geodetic astron­ omy including orbital theory and geodynamical phenomena. Since 1986, Dr. Lichteneg...

  7. Sobre el ciclo maya de 819 días

    Directory of Open Access Journals (Sweden)

    Huberto Quiñones Garza

    2011-01-01

    Full Text Available Algunos autores consideran que los mayas manejaban un ciclo de 819 días, que habría tenido un carácter mágico o ritual, sin descartar alguna manifestación astrológica o astronómica. Un enfoque que no ha sido tomado en cuenta hasta hoy, es el puramente aritmético, el posible interés del sacerdocio maya en este número como tal. Se especula aquí que el número 819 está relacionado con el valor de TT, además de la probable vinculación que esta cifra podría guardar con sus sistemas numérico y calendárico. Dos situaciones se vislumbran como importantes contribuciones, el planteamiento epistemológico implícito y los resultados obtenidos como información básica para futuras investigaciones dentro de la etnomatemática y la antropología.

  8. Modern Paradigm of Star Formation in the Galaxy

    Science.gov (United States)

    Sobolev, A. M.

    2017-06-01

    Understanding by the scientific community of the star formation processes in the Galaxy undergone significant changes in recent years. This is largely due to the development of the observational basis of astronomy in the infrared and submillimeter ranges. Analysis of new observational data obtained in the course of the Herschel project, by radio interferometer ALMA and other modern facilities significantly advanced our understanding of the structure of the regions of star formation, young stellar object vicinities and provided comprehensive data on the mass function of proto-stellar objects in a number of star-forming complexes of the Galaxy. Mapping of the complexes in molecular radio lines allowed to study their spatial and kinematic structure on the spatial scales of tens and hundreds of parsecs. The next breakthrough in this field can be achieved as a result of the planned project “Spektr-MM” (Millimetron) which implies a significant improvement in angular resolution and sensitivity. The use of sensitive interferometers allowed to investigate the details of star formation processes at small spatial scales - down to the size of the solar system (with the help of the ALMA), and even the Sun (in the course of the space project “Spektr-R” = RadioAstron). Significant contribution to the study of the processes of accretion is expected as a result of the project “Spektr-UV” (WSO-UV = “World Space Observatory - Ultraviolet”). Complemented with significant theoretical achievements obtained observational data have greatly promoted our understanding of the star formation processes.

  9. Comment on ‘Gravitational lensing of massive particles in Schwarzschild gravity’ (2016 Class. Quantum Grav. 33 175014)

    Science.gov (United States)

    Zakharov, Alexander F.

    2018-01-01

    Recently, Liu et al published a paper (2016 Class. Quantum Grav. 33 175014). In the abstract, the authors claimed as a key result of the paper that a particle sphere is found for the Schwarzschild black hole (BH), with its radius as a simple function of the particle velocity and proportional to the BH mass. Usually, if there are no references for the result it is assumed that the result was obtained originally in the paper; but this is not the case for the quoted paper. The concept of a particle sphere was introduced by Mielnik and Plebański (1962 Acta Phys. Pol. 21 239) and a simple derivation of the critical impact parameter was given in Zakharov A F (1988 Sov. Astron. 32 456 and Zakharov A F 1994 Class. Quantum Grav. 11 1027). We show that in slightly different notations, equation (17) for the critical impact parameter in Liu X et al (2016 Class. Quantum Grav. 33 175014) coincides with equation (12) in Zakharov (1994 Class. Quantum Grav. 11 1027) and with the corresponding equation (10.10) in Mielnik and Plebański (1962 Acta Phys. Pol. 21 239).

  10. Model shape and spin direction of the asteroid 2011 UW158

    Science.gov (United States)

    Silva, José; Monteiro, Filipe; Tamayo, Francisco

    2017-10-01

    We determinate the spin direction and convex model shape of the Near Earth Asteroid 2011 UW158 using the lightcurves from the Minor Planet Center database and obtained from the San Pedro Mártir observatory (Ensenada, Baja California, Mexico) and the Observatório Astronômico do Sertão de Itaparica (Itacuruba, Pernambuco, Brazil) by mean of the light-curve inversion technique.The shape model was compared with the radar images obtained from the 230-foot-wide Deep Space Network antenna at Goldstone, California, in concert with the National Radio Astronomy Observatory's 330-foot Green Bank Telescope in July 2015 and with the spin direction published for Carbognani et. al (2016).We found that the spin direction given for Carbognani et al. does not correspond with the visual geometry observed from the radar images. Also, we try to minimize the number of lightcurves that reproduce the shape in a robust way, with the objective of to plan future observations of asteroids better and prioritize time.

  11. Distribución espacial de órbitas con diferentes grados de caoticidad en modelos autoconsistentes de satélites galácticos

    Science.gov (United States)

    Muzzio, J. C.; Mosquera, M.

    En trabajos anteriores (Carpintero et al., Cel. Mech. Dynam. Astron. 85, 247, 2003), mostramos que las órbitas caóticas son muy importantes en los satélites galácticos. Sin embargo, los únicos modelos autoconsistentes de los que se disponía para ellos eran los de Heggie-Ramamani, cuya función de distribución depende sólo de la energía por lo que no mostraban diferencias entre las distribuciones de sus órbitas regulares y caóticas. Ahora, mediante una aproximación cuadrupolar, hemos logrado construir modelos autoconsistentes de satélites galácticos con distribuciones de velocidades anisotrópicas (lo que indica que sus funciones de distribución no dependen sólo de la energía) y hemos logrado revelar las diferencias entre las estructuras espaciales de las órbitas de distinta caoticidad.

  12. The Science Teachers and Their way of Thinking about Astronomy. (Spanish Title: Los Profesores de Ciencias y Sus Formas de Pensar la Astronomía.) Os Professores de Ciências e Suas Formas de Pensar a Astronomia

    Science.gov (United States)

    Leite, Cristina; Hosoume, Yassuko

    2007-12-01

    The research presented in this article is about the way science teachers from Elementary School think about astronomical elements. Its methodology is based on semi-structured interviews, which were video recorded. The research is centered in a three-dimensional perspective of astronomical Earth, the Sun, the Moon, the planets and the stars, and also the conceptions about sky and Universe. The esults indicate a Universe that contains: Sun, stars, planets and Moon; where the Solar System is a little part of the whole. Sometimes they think that the Solar System is the Universe. The objects are in the sky or in the Universe, which, for many of them, is only the space above the Earth. The flat shape of astronomical objects and the spatial structure of the Universe are striking features. Many of them think that Sun and stars are different: the Sun is a hot object and the stars are cold ones. These results worry us and they certainly indicate how urgent it is to plan Professional Development in Astronomy for teachers, after all the PCN's emphasize that this subject is important to be taught. El objeto de investigación de este artículo es la manera de pensar sobre los elementos de la Astronomía de los profesores de Ciencias en la enseñanza fundamental. La metodología consiste en entrevistas semi-estructuradas, filmadas en video y centradas en la tridimensionalidad de los elementos astronómicos, para posibilitar un mapeamiento de las concepciones sobre las formas y dimensiones de la Tierra, del Sol, de la Luna, de los planetas y de las estrellas, como también de la concepción de cielo y de Universo en su totalidad. Los resultados indican un Universo conteniendo: Sol, estrellas, planetas y Luna, donde el Sistema Solar se ubica como parte. Algunas veces, el Universo es concebido como el propio Sistema Solar. Los objetos están en el cielo o en el Universo, que, para muchos, se restringe al espacio que está arriba de la Tierra. La forma plana de los objetos astron

  13. The "Cool Algol" BD+05 706 : Photometric observations of a new eclipsing double-lined spectroscopic binary

    Science.gov (United States)

    Marschall, L. A.; Torres, G.; Neuhauser, R.

    1998-05-01

    BVRI Observations of the star BD+05 706, carried out between January, 1997, and April 1998 using the 0.4m reflector and Photometrics CCD camera at the Gettysburg College Observatory, show that the star is an eclipsing binary system with a light curve characteristic of a class of semi-detached binaries known as the "cool Algols". These results are in good agreement with the previous report of BD+05 706 as a cool Algol by Torres, Neuhauser, and Wichmann,(Astron. J., 115, May 1998) who based their classification on the strong X-ray emission detected by Rosat and on a series of spectroscopic observations of the radial velocities of both components of the system obtained at the Oak Ridge Observatory, the Fred L. Whipple Observatory, and the Multiple Mirror Telescope. Only 10 other examples of cool Algols are known, and the current photometric light curve, together with the radial velocity curves obtained previously, allows us to derive a complete solution for the physical parameters of each component, providing important constraints on models for these interesting systems.

  14. A Deep Arecibo Spectral Scan of Arp 220

    Science.gov (United States)

    Vick, Michelle; Ghosh, T.; Salter, C. J.; Minchin, R. F.

    2014-01-01

    A deep spectral scan of the prototype Ultra Luminous Infra-Red Galaxy (ULIRG), Arp 220, has been made over the frequency range 1.1 to 10.0 GHz using the 305-m Arecibo telescope. These new observations supersede a previous shallow scan of Arp 220 (Salter et al., 2008, Astron. J., 136, 389). The spectral lines seen in the previous scan were all re-detected with greatly improved signal-to-noise ratio. These lines include hydrogen cyanide (HCN v2=1) in absorption, formaldehyde (H2CO) in emission at 4.83 GHz, and hydroxyl (OH) in emission at 1.6 GHz and absorption at 4.7, 6.0 and 7.8 GHz. In addition, a large number of hydrogen recombination lines were detected, as was the H2CO line at 4.955 GHz, and two lines that are identified with excited transitions of methylidyne (CH) at 4.848 and 4.870 GHz. The identification of other possible detections is on-going.

  15. Design of VLBI Array in South America

    Science.gov (United States)

    Carrara, E. A.; Abraham, Z.

    1990-11-01

    RESUMEN. Estudiamos la localizaci6n 6ptima de estaciones de \\ ras' en territorlo brasileno. Con una red VLBI de estaciones reales y ficti- cias simulamos observaciones. Se usan los datos generados de estps ex- perimentos para obtener Ia distribuci6n de brillo de radiofuentes fic- ticias por medlo de tecaicas de mapeo bIbrido. Se concluye que l mejor localizaci6n de estacionee'VLBI futuras, tomando en cuenta las estacio- nes de EUA y de Europa, se encuentra en el Norte-Noreste de razll. El analisis de los datos se hizo con los programas de CALTECH, los cuales estan instalados en una computadora VAX del Departamento de Astronomla del Instituto Astron6mico y Geoflsico de la Universidad de Sa"'o Paulo. ABSTRACT: In this work we study the optimum localization for future VLBI stations in the Brazilian territory. With a VLBI network of real and fictitious stations we make simulations of observations. The data generated in these experiments are used to obtain brightness distribution of a fictitious radio source by the hybrid mapping techniques. We conclude that the best localization of a future VLBI station taking into account the addition of US and European Stations, is roughly in North-Northeast sites in Brazil. The analysis of the data is made with the software of CALTECH, which is installed in the VAX computer of the Astronomy Department of Instituto e Geofisico - USP. Key `{` : INSTRUMENTS - INTERFEROMETRY

  16. Velocidades radiales en Collinder 121

    Science.gov (United States)

    Arnal, M.; Morrell, N.

    Se han llevado a cabo observaciones espectroscópicas de unas treinta estrellas que son posibles miembros del cúmulo abierto Collinder 121. Las mismas fueron realizadas con el telescopio de 2.15m del Complejo Astronómico El Leoncito (CASLEO). El análisis de las velocidades radiales derivadas del material obtenido, confirma la realidad de Collinder 121, al menos desde el punto de vista cinemático. La velocidad radial baricentral (LSR) del cúmulo es de +17 ± 3 km.s-1. Esta velocidad coincide, dentro de los errores, con la velocidad radial (LSR) de la nebulosa anillo S308, la cual es de ~20 ± 10 km.s-1. Como S308 se encuentra físicamente asociada a la estrella Wolf-Rayet HD~50896, es muy probable que esta última sea un miembro de Collinder 121. Desde un punto de vista cinemático, la supergigante roja HD~50877 (K3Iab) también pertenecería a Collinder 121. Basándonos en la pertenencia de HD~50896 a Collinder 121, y en la interacción encontrada entre el viento de esta estrella y el medio interestelar circundante a la misma, se estima para este cúmulo una distancia del orden de 1 kpc.

  17. Relativistic viscous hydrodynamics for heavy-ion collisions with ECHO-QGP

    Energy Technology Data Exchange (ETDEWEB)

    Del Zanna, L. [Universita di Firenze, Dipartimento di Fisica e Astronomia, Sesto Fiorentino (Italy); INFN, Sezione di Firenze, Sesto Fiorentino (Italy); INAF, Osservatorio Astrofisico di Arcetri, Firenze (Italy); Chandra, V. [INFN, Sezione di Firenze, Sesto Fiorentino (Italy); Inghirami, G. [Universita di Firenze, Dipartimento di Fisica e Astronomia, Sesto Fiorentino (Italy); INFN, Sezione di Firenze, Sesto Fiorentino (Italy); Rolando, V.; Pagliara, G.; Drago, A. [Universita di Ferrara, Dipartimento di Fisica e Scienze della Terra, Ferrara (Italy); INFN, Sezione di Ferrara, Ferrara (Italy); Beraudo, A. [Theory Unit, CERN, Physics Department, Geneve (Switzerland); De Pace, A. [INFN, Sezione di Torino, Torino (Italy); Becattini, F. [Universita di Firenze, Dipartimento di Fisica e Astronomia, Sesto Fiorentino (Italy); INFN, Sezione di Firenze, Sesto Fiorentino (Italy); Frankfurt Institute for Advanced Studies, Frankfurt am Main (Germany)

    2013-08-15

    We present ECHO-QGP, a numerical code for (3+1)-dimensional relativistic viscous hydrodynamics designed for the modeling of the space-time evolution of the matter created in high-energy nuclear collisions. The code has been built on top of the Eulerian Conservative High-Order astrophysical code for general relativistic magneto-hydrodynamics (Del Zanna et al. in Astron. Astrophys. 473:11, 2007) and here it has been upgraded to handle the physics of the Quark-Gluon Plasma. ECHO-QGP features second-order treatment of causal relativistic viscosity effects both in Minkowskian and in Bjorken coordinates; partial or complete chemical equilibrium of hadronic species before kinetic freeze-out; initial conditions based on the Glauber model, including a Monte-Carlo routine for event-by-event fluctuating initial conditions; a freeze-out procedure based on the Cooper-Frye prescription. The code is extensively validated against several test problems and results always appear accurate, as guaranteed by the combination of the conservative (shock-capturing) approach and the high-order methods employed. ECHO-QGP can be extended to include evolution of the electromagnetic fields coupled to the plasma. (orig.)

  18. Interstellar scintillations of PSR B1919+21: space-ground interferometry

    Science.gov (United States)

    Shishov, V. I.; Smirnova, T. V.; Gwinn, C. R.; Andrianov, A. S.; Popov, M. V.; Rudnitskiy, A. G.; Soglasnov, V. A.

    2017-07-01

    We carried out observations of pulsar PSR B1919+21 at 324 MHz to study the distribution of interstellar plasma in the direction of this pulsar. We used the RadioAstron (RA) space radio telescope, together with two ground telescopes: Westerbork (WB) and Green Bank (GB). The maximum baseline projection for the space-ground interferometer was about 60 000 km. We show that interstellar scintillation of this pulsar consists of two components: diffractive scintillations from inhomogeneities in a layer of turbulent plasma at a distance z1 = 440 pc from the observer or homogeneously distributed scattering material to the pulsar; and weak scintillations from a screen located near the observer at z2 = 0.14 ± 0.05 pc. Furthermore, in the direction to the pulsar we detected a prism that deflects radiation, leading to a shift in observed source position. We show that the influence of the ionosphere can be ignored for the space-ground baseline. Analysis of the spatial coherence function for the space-ground baseline (RA-GB) yielded a scattering angle in the observer plane of θscat = 0.7 mas. An analysis of the time-frequency correlation function for weak scintillations yielded an angle of refraction in the direction to the pulsar θref, 0 = 110 ms and a distance to the prism zprism ≤ 2 pc.

  19. Distribution of interstellar plasma in the direction of PSR B0525+21 from data obtained on a ground-space interferometer

    Science.gov (United States)

    Andrianov, A. S.; Smirnova, T. V.; Shishov, V. I.; Gwinn, C.; Popov, M. V.

    2017-06-01

    Observations on the RadioAstron ground-space interferometer with the participation of the Green Bank and Arecibo ground telescopes at 1668 MHz have enabled studies of the characteristics of the interstellar plasma in the direction of the pulsar PSR B0525+21. The maximum projected baseline for the ground-space interferometer was 233 600 km. The scintillations in these observations were strong, and the spectrum of inhomogeneties in the interstellar plasma was a power law with index n = 3.74, corresponding to a Kolmogorov spectrum. A new method for estimating the size of the scattering disk was applied to estimate the scattering angle (scattering disk radius) in the direction toward PSR B0525+21, θ scat = 0.028 ± 0.002 milliarcsecond. The scattering in this direction occurs in a plasma layer located at a distance of 0.1 Z from the pulsar, where Z is the distance from the pulsar to the observer. For the adopted distance Z = 1.6 kpc, the screen is located at a distance of 1.44 kpc from the observer.

  20. Eventos de Desconexão no Cometa P/Halley sob a Ótica do Modelo de Reconexão Magnética

    Science.gov (United States)

    Voelzke, M. R.; Matsuura, O. T.

    1998-08-01

    determinam o tempo de desconexão a partir de um movimento linear constantemente acelerado (Yi et al., 1994). A velocidade de um DE para outro varia enormemente. - Brandt, J.C., Niedner, M.B.Jr. and Rahe, J., (1992) The International Halley Watch Atlas of Large-Scale Phenomena (printed by: Johnson Printing Co., Boulder, CO), University of Colorado-Boulder. - Celnik, W.E., Koczet, P., Schlosser, W., Schulz, R., Svejda, P. and Weissbauer, K., (1988) Astron. Astrophys. Suppl. Ser. 72, 89. - Delva, M., Schwingenschuh, K., Niedner, M.B.Jr. and Gringauz, K.I., (1991) Planet. Space Sci. 39, Number 5, 697. - Hoeksema, J.T., (1989) Adv. Space Res. 9, 141. - Jockers, K., (1985) Astron. Astrophys. Suppl. Ser. 62, 791. - Niedner, M.B.Jr. and Brandt, J.C., (1979) Astrophys. J. 234, 723. - Voelzke, M.R. and Matsuura, O.T., (1988) Planet. Space Sci. 46, 835. - Yi, Y., Caputo, M.F. and Brandt, J.C., (1994) Planet. Space Sci. 42, Number 9, 705.

  1. An investigation of the low-ΔV near-Earth asteroids (341843) 2008 EV5 and (52381) 1993 HA. Two suitable targets for the ARM and MarcoPolo-M5 space missions

    Science.gov (United States)

    Perna, D.; Popescu, M.; Monteiro, F.; Lantz, C.; Lazzaro, D.; Merlin, F.

    2017-01-01

    Context. The Asteroid Redirect Mission (ARM) under development by NASA is being planned to collect a multi-meter boulder from a near-Earth asteroid (NEA), and to bring it to the cis-lunar space in the mid-2020's for future study and exploitation by a crewed mission. The MarcoPolo-M5 project is being proposed in 2016 for the M5 mission opportunity by ESA, to bring back to Earth a sample from a very primitive D-type NEA. As D-types are very rare within the NEA population, considerable effort is still in progress to characterize easily accessible targets with unknown surface composition, in order to discover further asteroids that belong to this taxonomic group. Aims: We aim to further characterize the physical properties of two optimal targets for sample return space missions, the low-ΔV NEAs (341843) 2008 EV5 and (52381) 1993 HA. The asteroid 2008 EV5 is the baseline target of ARM, but only one spectrum of this object exists in the literature. The asteroid 1993 HA is a very favourable target for a space mission based on its dynamical properties: here we intend to assess if it is a suitable target for MarcoPolo-M5. Methods: We obtained visible spectroscopy of 2008 EV5 with the FORS2 instrument at ESO-VLT (Paranal, Chile), at different rotational phases. We also obtained visible and near-infrared spectroscopy of 1993 HA, using the EFOSC2 and SOfI instruments at ESO-NTT (La Silla, Chile). Visible photometry of 1993 HA was carried out within the IMPACTON project at the Observatório Astronômico do Sertão de Itaparica (Itacuruba, Brazil). Results: Our new observations are in agreement with the C-type classification of 2008 EV5, which is a requirement for the ARM mission. We obtained five visible spectra which do not show any variability within the limits of noise, suggesting a homogeneous surface. We obtained the first ever spectroscopic dataset ( 0.4-1.6 μm) for 1993 HA, finding a featureless, red-sloped behaviour typical of D-types (a T or X classification is also

  2. El Sistema de Referencia Celeste convencional de la IAU

    Science.gov (United States)

    Arias, E. F.

    La Unión Astronómica Internacional (IAU) recomendó la adopción de un nuevo sistema de referencia celeste baricéntrico cuyo plano fundamental y origen de ascensiones rectas estén próximos, respectivamente, al ecuador y equinoccio dinámicos J2000.0. El nuevo sistema de referencia estará materializado por las posiciones J2000.0 de radiofuentes extragalácticas determinadas con la técnica de interferometría de larga línea de base (VLBI). El Working Group on Reference Frames de la IAU (WGRF) decidió adoptar (Grasse, 1995) al sistema de referencia celeste extragaláctico del Servicio Internacional de la Rotación Terrestre (IERS) como futuro sistema de referencia celeste convencional bajo el nombre International Celestial Reference System (ICRS) y encomendó su mantenimiento futuro al IERS. El marco de referencia que materializará al ICRS contiene posiciones precisas J2000.0 de más de 600 radiofuentes extragalácticas. Las coordenadas fueron ajustadas en una única solución VLBI en la cual se incluyeron todas las observaciones realizadas hasta octubre de 1995 con la técnica de adquisición de datos VLBI Mark III. Para minimizar los errores sistemáticos que pueden afectar la calidad del marco de referencia se introdujeron mejoras sustanciales en la modelización y en la selección de datos. Un subconjunto de objetos del marco de referencia se utilizó para referir las posiciones estelares determinadas con el satélite astrométrico Hipparcos al ICRS.

  3. Observações no âmbito dos "additional programs" do satélite COROT

    Science.gov (United States)

    Janot Pacheco, E.

    2003-08-01

    O satélite Fraco-europeu COROT fará fotometria de altissima precisão (pretende-se atingir uma parte em um milhão), grande campo (3x3 graus) e por longos períodos, de duas regiões pré-determinadas do céu, com 10 graus de raio. Suas finalidades básicas serão estudos em sismologia estelar e a procura de exoplanetas. A comunidade astronômica brasileira participará dessa missão espacial, com direitos iguais aos dos parceiros europeus. Isso se deve a que o satélite utilizará a estação de recepção de dados de Natal (INPE), 5 a 6 brasileiros participarão das equipes de software e cientistas do país atuarão na fase de pré-lançamento. Apresentamos nesta comunicação sugestões para a preparação de propostas de observações com COROT, no âmbito dos Programas Adicionais, que contemplam outros projetos que não de sismologia ou exoplanetas. As últimas definições técnicas e decisões tomadas na 4th Corot Week de junho último serão igualmente apresentadas, em particular quanto às regiões de observação escolhidas e quanto aos procedimentos a seguir para se propor observações.

  4. Análisis del futuro marco de referencia internacional

    Science.gov (United States)

    Cionco, G. R.; Arias, E. F.

    La técnica de interferometría de muy larga línea de base (VLBI) se aplica hoy a la astrometría para el cálculo de posiciones precisas de radiofuentes extragalácticas. Por tratarse de objetos lejanos, sus movimientos propios aparentes pueden considerarse nulos; esta propiedad hace que los catálogos de radiofuentes extragalácticas VLBI constituyan la mejor materialización de un sistema de referencia celeste inercial definido cinemáticamente. La Unión Astronómica Internacional (IAU) recomendó la adopción de un nuevo sistema de referencia celeste internacional materializado por las coordenadas ecuatoriales de objetos extragalácticos observados con le técnica VLBI. Para superar la precisión astrométrica actual es necesaria una mejora en la modelización de aquellos fenómenos que pueden introducir desviaciones sistemáticas en el marco de referencia celeste. El objetivo de este trabajo es poner de manifiesto las sistematicidades presentes en los distintos marcos de referencia elaborados con el próposito de materializar el nuevo sistema de referencia celeste de la IAU. Para la comparación de los distintos marcos de referencia se propone un modelo de tres rotaciones diferenciales más un término lineal que procura absorber los efectos sistemáticos presentes en las coordenadas. Se analiza igualmente la estabilidad de la solución cuando se utilizan distintos conjuntos de objetos de definición.

  5. OV-Wav: um novo pacote para análise multiescalar em astronomia

    Science.gov (United States)

    Pereira, D. N. E.; Rabaça, C. R.

    2003-08-01

    Wavelets e outras formas de análise multiescalar têm sido amplamente empregadas em diversas áreas do conhecimento, sendo reconhecidamente superiores a técnicas mais tradicionais, como as análises de Fourier e de Gabor, em certas aplicações. Embora a teoria dos wavelets tenha começado a ser elaborada há quase trinta anos, seu impacto no estudo de imagens astronômicas tem sido pequeno até bem recentemente. Apresentamos um conjunto de programas desenvolvidos ao longo dos últimos três anos no Observatório do Valongo/UFRJ que possibilitam aplicar essa poderosa ferramenta a problemas comuns em astronomia, como a remoção de ruído, a detecção hierárquica de fontes e a modelagem de objetos com perfis de brilho arbitrários em condições não ideais. Este pacote, desenvolvido para execução em plataforma IDL, teve sua primeira versão concluída recentemente e está sendo disponibilizado à comunidade científica de forma aberta. Mostramos também resultados de testes controlados ao quais submetemos os programas, com a sua aplicação a imagens artificiais, com resultados satisfatórios. Algumas aplicações astrofísicas foram estudadas com o uso do pacote, em caráter experimental, incluindo a análise da componente de luz difusa em grupos compactos de galáxias de Hickson e o estudo de subestruturas de nebulosas planetárias no espaço multiescalar.

  6. Apoastron shift constraints on dark matter distribution at the Galactic Center

    Science.gov (United States)

    Zakharov, A. F.; Nucita, A. A.; de Paolis, F.; Ingrosso, G.

    2007-09-01

    The existence of dark matter (DM) at scales of a few parsecs down to ≃10-5pc around the centers of galaxies and, in particular, in the Galactic Center region has been considered in the literature. Under the assumption that such a DM clump, principally constituted by nonbaryonic matter (like weakly interacting massive particles) does exist at the center of our galaxy, the study of the γ-ray emission from the Galactic Center region allows us to constrain both the mass and the size of this DM sphere. Further constraints on the DM distribution parameters may be derived by observations of bright infrared stars around the Galactic Center. Hall and Gondolo [J. Hall and P. Gondolo, Phys. Rev. D 74, 063511 (2006)PRVDAQ0556-282110.1103/PhysRevD.74.063511] used estimates of the enclosed mass obtained in various ways and tabulated by Ghez et al. [A. M. Ghez , Astron. Nachr. 324, 527 (2003); ASNAAN0004-633710.1002/asna.200385103A. M. Ghez , Astrophys. J.ASJOAB0004-637X 620, 744 (2005)10.1086/427175]. Moreover, if a DM cusp does exist around the Galactic Center it could modify the trajectories of stars moving around it in a sensible way depending on the DM mass distribution. Here, we discuss the constraints that can be obtained with the orbit analysis of stars (as S2 and S16) moving inside the DM concentration with the present and next generations of large telescopes. In particular, consideration of the S2 star apoastron shift may allow improving limits on the DM mass and size.

  7. Astronomical elements in the religious and funerary world of the ancient Iberians

    Directory of Open Access Journals (Sweden)

    Esteban, César

    2002-12-01

    Full Text Available We present an archaeoastronomical study of 16 sacred and funerary Iberian sites. The work is based on the analysis of the orientation of architectural structures as well as the horizon surrounding each site. Seven of the sites surveyed (44% of them show relevant astronomical relations, mainly to the sunrise or sunset at the equinoxes. We find that most of the iberian sacred buildings not dedicated to cults of domestic character are oriented to the part of the horizon where the sunrise (or moonrise takes place. This pattern of orientations is similar to those shown by Greek, pre- Roman African and perhaps Phoenician and Punic temples, and definetively different to Roman and Etruscan patterns.

    Se presenta un análisis arqueoastronómico de la orientación de las estructuras arquitectónicas así como del horizonte que rodea a 16 yacimientos ibéricos de carácter religioso y funerario. Siete de los lugares estudiados (un 44% presentan relaciones astronómicas relevantes, principalmente con el orto u ocaso solar en los equinoccios. Por otra parte, se obtiene que la mayoría de los edificios de culto ibéricos no domésticos se encuentran orientados hacia la zona del horizonte donde se producen los ortos del sol (o la luna. Este patrón de orientaciones es similar al mostrado por los templos griegos, los africanos prerromanos y quizás también los púnicos y fenicios, pero diferente al romano y al etrusco.

  8. Autonomous landing guidance system validation

    Science.gov (United States)

    Bui, Long Q.; Franklin, Michael R.; Taylor, Christopher; Neilson, Graham

    1997-06-01

    ALG is a combination of raster imaging sensor, head-up displays, flight guidance and procedures which allow pilots to perform hand flown aircraft maneuvers in adverse weather, at night, or in low visibility conditions at facilities with minimal or no ground aids. Maneuvers in the context of ALG relate to takeoff, landing, rollout, taxi and terminal parking. Commercial needs are driven by potential revenue savings since today only 43 Type III and 80 Type II instrumented landing system (ILS) runway ends in the United States are equipped for lower minimum flight operations. Additionally, most of these ILS facilities are clustered at major gateway airports which further impacts on dispatch authority and general ATC regional delays. Infrastructure consists to upgrade additional runways must not only account for the high integrity ground instrumentation, but also the installation of lights and markers mandated for Cat III operations. The military services ability to train under realistic battlefield conditions, to project power globally in support of national interests, while providing humanitarian aid, is significantly impaired by the inability to conduct precision approaches and landings in low visibility conditions to either instrumented runways or to a more tactical environment with operations into and out of unprepared landing strips, particularly when time does not permit deployment of ground aids and the verification of their integrity. Recently, Lear Astronics, in cooperation with Consortium members of the ALG Program, concluded a flight test program which evaluated the utility of the ALG system in meeting both civil and military needs. Those results are the subject of this paper.

  9. Towards Perfect Water Line Intensities

    Science.gov (United States)

    Lodi, L.; Tennyson, J.

    2012-06-01

    Over the last ten years the increased availability of computational resources and the steady refinement of theoretical methods have permitted more and more accurate first principle calculations of water-vapor spectra as exemplified, e.g., by the very successful BT2 line list both line positions and intensities, a reliable dipole moment surface (DMS), affecting line intensities. It is also very useful to several application to give reasonable uncertainty bars for computed quantities, an aspect which traditionally has received little attention. We report here recent progress leading to very accurate room-temperature linelists covering the range 0.05-20 000 cm-1, complete with uncertainty bars, for the H_218O and H_217O water isotopologues Line intensities were produced using a recent DMS produced by our group which is capable of giving line intensites accurate to 1% for most medium and strong transitions. Line positions are based if possible on the experimentally derived energy levels recently produced by a IUPAC task group and have a typical accuracy of 0.0002 cm-1; when experimentally derived energy levels are unavailable calculated line position are provided, with an accuracy of the order of 0.2 cm-1. An extension to the main isotopologue H_216O is currently underway. R. J. Barber, J. Tennyson, G. J. Harris and R. N. Tolchenov, Mon. Not. R. Astron. Soc. {368}, 1087-1094 (2006). L. Lodi and J. Tennyson, J. Quant. Spectrosc. Radiat. Trans. (2012), doi:10.1016/j.jqsrt.2012.02.023 L. Lodi, J. Tennyson and O. L. Polyansky, J. Chem. Phys. {135}, 034113 (2011). J. Tennyson at al., J. Quant. Spectrosc. Radiat. Trans. {110}, 573-96 (2009).

  10. Composition of near-Earth Asteroid 2008 EV5: Potential target for robotic and human exploration

    Science.gov (United States)

    Reddy, Vishnu; Le Corre, Lucille; Hicks, Michael; Lawrence, Kenneth; Buratti, Bonnie J.; Abell, Paul A.; Gaffey, Michael J.; Hardersen, Paul S.

    2012-11-01

    We observed Potentially Hazardous Asteroid (PHA) 2008 EV5 in the visible (0.30-0.92 μm) and near-IR (0.75-2.5 μm) wavelengths to determine its surface composition. This asteroid is especially interesting because it is a potential target for two sample return mission proposals (Marco Polo-R and Hayabusa-2) and human exploration due to its low delta-v for rendezvous. The spectrum of 2008 EV5 is essentially featureless with exception of a weak 0.48-μm spin-forbidden Fe3+ absorption band. The spectrum also has an overall blue slope. The albedo of 2008 EV5 remains uncertain with a lower limit at 0.05 and a higher end at 0.20 based on thermal modeling. The Busch et al. (Busch et al. [2011]. Icarus 212, 649-660) albedo estimate of 0.12 ± 0.04 is consistent with our thermal modeling results. The albedo and composition of 2008 EV5 are also consistent with a C-type taxonomic classification (Somers, J.M., Hicks, M.D., Lawrence, K.J. [2008]. Bull. Am. Astron. Soc. 40, 440). The best spectral match is with CI carbonaceous chondrites similar to Orgueil, which also have a weak 0.48-μm feature and an overall blue slope. This 0.48-μm feature is also seen in the spectrum of magnetite. The albedo of CI chondrites is at the lower limit of our estimated range for the albedo of 2008 EV5.

  11. Frozen-wave instability in near-critical hydrogen subjected to horizontal vibration under various gravity fields.

    Science.gov (United States)

    Gandikota, G; Chatain, D; Amiroudine, S; Lyubimova, T; Beysens, D

    2014-01-01

    The frozen-wave instability which appears at a liquid-vapor interface when a harmonic vibration is applied in a direction tangential to it has been less studied until now. The present paper reports experiments on hydrogen (H2) in order to study this instability when the temperature is varied near its critical point for various gravity levels. Close to the critical point, a liquid-vapor density difference and surface tension can be continuously varied with temperature in a scaled, universal way. The effect of gravity on the height of the frozen waves at the interface is studied by performing the experiments in a magnetic facility where effective gravity that results from the coupling of the Earth's gravity and magnetic forces can be varied. The stability diagram of the instability is obtained. The experiments show a good agreement with an inviscid model [Fluid Dyn. 21 849 (1987)], irrespective of the gravity level. It is observed in the experiments that the height of the frozen waves varies weakly with temperature and increases with a decrease in the gravity level, according to a power law with an exponent of 0.7. It is concluded that the wave height becomes of the order of the cell size as the gravity level is asymptotically decreased to zero. The interface pattern thus appears as a bandlike pattern of alternate liquid and vapor phases, a puzzling phenomenon that was observed with CO2 and H2 near their critical point in weightlessness [Acta Astron. 61 1002 (2007); Europhys. Lett. 86 16003 (2009)].

  12. Realistic estimation for the detectability of dark matter subhalos using Fermi-LAT catalogs

    Science.gov (United States)

    Calore, Francesca; De Romeri, Valentina; Di Mauro, Mattia; Donato, Fiorenza; Marinacci, Federico

    2017-09-01

    Numerical simulations of structure formation have made remarkable progress in recent years, in particular due to the inclusion of baryonic physics evolving with the dark matter component. We generate Monte Carlo realizations of the dark matter subhalo population based on the results of the recent hydrodynamical simulation suite of Milky Way-sized galaxies [F. Marinacci, R. Pakmor, and V. Springel, Mon. Not. R. Astron. Soc. 437, 1750 (2014)., 10.1093/mnras/stt2003]. We then simulate the gamma-ray sky for both the setup of the 3FGL and 2FHL Fermi Large Area Telescope (LAT) catalogs, including the contribution from the annihilation of dark matter in the subhalos. We find that the flux sensitivity threshold strongly depends on the particle dark matter mass and, more mildly, also on its annihilation channel and the observation latitude. The results differ for the 3FGL and 2FHL catalogs, given their different energy thresholds. We also predict that the number of dark matter subhalos among the unassociated sources is very small. A null number of detectable subhalos in the Fermi-LAT 3FGL catalog would imply upper limits on the dark matter annihilation cross section into b b ¯ of 2 ×10-26(5 ×10-25) cm3 /s with MDM=50 (1000 ) GeV . We find less than one extended subhalo in the Fermi-LAT 3FGL catalog. As a matter of fact, the differences in the spatial and mass distribution of subhalos between hydrodynamic and dark matter-only runs do not have significant impact on the detectability of dark subhalos in gamma rays.

  13. Cosmic Rays in Thunderstorms

    Science.gov (United States)

    Buitink, Stijn; Scholten, Olaf; van den Berg, Ad; Ebert, Ute

    2013-04-01

    Cosmic Rays in Thunderstorms Cosmic rays are protons and heavier nuclei that constantly bombard the Earth's atmosphere with energies spanning a vast range from 109 to 1021 eV. At typical altitudes up to 10-20 km they initiate large particle cascades, called extensive air showers, that contain millions to billions of secondary particles depending on their initial energy. These particles include electrons, positrons, hadrons and muons, and are concentrated in a compact particle front that propagates at relativistic speed. In addition, the shower leaves behind a trail of lower energy electrons from ionization of air molecules. Under thunderstorm conditions these electrons contribute to the electrical and ionization processes in the cloud. When the local electric field is strong enough the secondary electrons can create relativistic electron run-away avalanches [1] or even non-relativistic avalanches. Cosmic rays could even trigger lightning inception. Conversely, strong electric fields also influence the development of the air shower [2]. Extensive air showers emit a short (tens of nanoseconds) radio pulse due to deflection of the shower particles in the Earth's magnetic field [3]. Antenna arrays, such as AERA, LOFAR and LOPES detect these pulses in a frequency window of roughly 10-100 MHz. These systems are also sensitive to the radiation from discharges associated to thunderstorms, and provide a means to study the interaction of cosmic ray air showers and the electrical processes in thunderstorms [4]. In this presentation we discuss the involved radiation mechanisms and present analyses of thunderstorm data from air shower arrays [1] A. Gurevich et al., Phys. Lett. A 165, 463 (1992) [2] S. Buitink et al., Astropart. Phys. 33, 1 (2010) [3] H. Falcke et al., Nature 435, 313 (2005) [4] S. Buitink et al., Astron. & Astrophys. 467, 385 (2007)

  14. Cassini ISS Observations of Jupiter: An Exoplanet Perspective

    Science.gov (United States)

    West, Robert A.; Knowles, Benjamin

    2017-10-01

    Understanding the optical and physical properties of planets in our solar system can guide our approach to the interpretation of observations of exoplanets. Although some work has already been done along these lines, there remain low-hanging fruit. During the Cassini Jupiter encounter, the Imaging Science Subsystem (ISS) obtained an extensive set of images over a large range of phase angles (near-zero to 140 degrees) and in filters from near-UV to near-IR, including three methane bands and nearby continuum. The ISS also obtained images using polarizers. Much later in the mission we also obtained distant images while in orbit around Saturn. Some of these data have already been studied to reveal phase behavior (Dyudina et al., Astrophys. J.822, DOI: 10.3847/0004-637X/822/2/76; Mayorga et al., 2016, Astron. J. 152, DOI: 10.3847/0004-6256/152/6/209). Here we examine rotational modulation to determine wavelength and phase angle dependence, and how these may depend on cloud and haze vertical structure and optical properties. The existence of an optically thin forward-scattering and longitudinally-homogeneous haze overlying photometrically-variable cloud fields tends to suppress rotational modulation as phase angle increases, although in the strong 890-nm methane band cloud vertical structure is important. Cloud particles (non-spherical ammonia ice, mostly) have very small polarization signatures at intermediate phase angles and rotational modulation is not apparent above the noise level of our instrument. Part of this work was performed by the Jet Propulsion Lab, Cal. Inst. Of Technology.

  15. Marriage of Electromagnetism and Gravity in an Extended Space Model and Astrophysical Phenomena

    Science.gov (United States)

    Andreev, V. A.; Tsipenyuk, D. Yu.

    2013-09-01

    The generalization of Einstein's special theory of relativity (SRT) is proposed. In this model the possibility of unification of scalar gravity and electromagnetism into a single unified field is considered. Formally, the generalization of the SRT is that instead of (1+3)-dimensional Minkowski space the (1+4)-dimensional extension G is considered. As a fifth additional coordinate the interval S is used. This value is saved under the usual Lorentz transformations in Minkowski space M, but it changes when the transformations in the extended space G are used. We call this model the extended space model (ESM). From a physical point of view our expansion means that processes in which the rest mass of the particles changes are acceptable now. If the rest mass of a particle does not change and the physical quantities do not depend on an additional variable S, then the electromagnetic and gravitational fields exist independently of each other. But if the rest mass is variable and there is a dependence on S, then these two fields are combined into a single unified field. In the extended space model a photon can have a nonzero mass and this mass can be either positive or negative. The gravitational effects such as the speed of escape, gravitational red shift and detection of light can be analyzed in the frame of the extended space model. In this model all these gravitational effects can be found algebraically by the rotations in the (1+4) dimensional space. Now it becomes possible to predict some future results of visible size of supermassive objects in our Universe due to new stage of experimental astronomy development in the RadioAstron Project and analyze phenomena is an explosion of the star V838 Mon.

  16. Expo 70 - Osaka, Japón

    Directory of Open Access Journals (Sweden)

    Editorial, Equipo

    1970-06-01

    Full Text Available The following pavillions at the Expo-70 in Osaka are outstanding. The West German Exhibit, with a structure reminiscent of an astronomical observatory. The U.R.R.S. Pavillion, which is 109 m high, and has a tubular support. The Motor Car Industry Display, which involves two units and a tent like roof. The Festival Palace, within the representative zone of the Exhibition, and houses the official ceremonies in honour of the participating nations. The Tashida IHI Pavillion, whose structure includes the use of 1,338 interconnected tetrapods. The Takara Group Display, which is an abstract concept, consisting of a large number of cube space forms. The firm Takenaka Komuten Co. Ltd. has taken a very active part in the construction of 28 buildings, both Japanese and foreign.Destacan en la EXPO-70 los siguientes pabellones: el pabellón de la Alemania Occidental, con su estructura en forma de cúpula para observaciones astronómicas; el de la U.R.S.S., de 109 m de altura y estructura tubular; el de la Industria Automovilística, que consta de dos unidades y presenta una cubierta en forma de tienda de campaña; el palacio de Festivales, que forma parte de la zona representativa de la exposición; en él se desarrollan los actos dedicados a las naciones participantes; el pabellón Toshiba IHI, en cuya estructura se emplearon un total de 1.338 tetrápodos ensamblados; el pabellón del grupo Takara, diseñado con una concepción abstracta —a base de cubos—. La empresa «Takenaka Komuten, Co. Ltd.», ha intervenido eficazmente en la construcción de 28 pabellones, japoneses y extranjeros.

  17. A deep search for the release of volcanic gases on Mars using ground-based high-resolution infrared and submillimeter spectroscopy: Sensitive upper limits for OCS and SO2

    Science.gov (United States)

    Khayat, A.; Villanueva, G. L.; Mumma, M. J.; Tokunaga, A. T.

    2017-11-01

    Recent volcanic activity has long been considered a distinct possibility that would place major constraints on the evolution of Mars' interior. Volcanic activity would result in the outgassing of sulfur-bearing species. As part of our multi-band search for active release of volcanic gases on Mars, we looked for carbonyl sulfide (OCS) at its combination band (ν1 +ν3) at 3.42 μ m (2924 cm-1), and sulfur dioxide (SO2) at 346.652 GHz, in two successive Mars years during its late Northern spring and mid Northern summer seasons (Ls= 43°-144°). The targeted volcanic districts, Tharsis and Syrtis Major, were observed during the two intervals, 15 Dec. 2011 to 6 Jan. 2012 in the first year, and 23 May 2014 to 12 June 2014 in the second year using the high resolution infrared spectrometer CSHELL on the NASA Infrared Telescope Facility, and the high resolution heterodyne receiver HARP at the James Clerk Maxwell Telescope atop Maunakea, Hawaii. No active release of such gases was detected, and we report 2σ upper limits of 1.8 ppbv and 3.1 ppbv for OCS and SO2, respectively, compared to 0.3 ppbv for SO2 (Encrenaz, T. et al. [2011] Astron. & Astrophys. 530, A37; Krasnopolsky, V.A. [2012] Icarus 217, 144-152) over the disk of Mars. Our retrieved upper limit on the SO2 outgassing rate of 156 tons/day (1.8 kg/s), corresponds to a mass rate of magma that is able to degas the SO2 of 104 kilotons/day (1200 kg/s), or 40,000 m3/day (0.46 m3/s). Our campaign places stringent limits on the concentration of sulfur-bearing species into the atmosphere of Mars.

  18. Measurements of Seismic Anisotropy in Synthetic Rocks with Controlled Crack Geometry and Different Crack Densities

    Science.gov (United States)

    Ding, Pinbo; Di, Bangrang; Wang, Ding; Wei, Jianxin; Li, Xiangyang

    2017-05-01

    Seismic anisotropy can help to extract azimuthal information for predicting crack alignment, but the accurate evaluation of cracked reservoir requires knowledge of degree of crack development, which is achieved through determining the crack density from seismic or VSP data. In this research we study the dependence of seismic anisotropy on crack density, using synthetic rocks with controlled crack geometries. A set of four synthetic rocks containing different crack densities is used in laboratory measurements. The crack thickness is 0.06 mm and the crack diameter is 3 mm in all the cracked rocks, while the crack densities are 0.00, 0.0243, 0.0486, and 0.0729. P and S wave velocities are measured by an ultrasonic investigation system at 0.5 MHz while the rocks are saturated with water. The measurements show the impact of crack density on the P and S wave velocities. Our results are compared to the theoretical prediction of Chapman (J App Geophys 54:191-202, 2003) and Hudson (Geophys J R Astron Soc 64:133-150, 1981). The comparison shows that measured velocities and theoretical results are in good quantitative agreement in all three cracked rocks, although Chapman's model fits the experimental results better. The measured anisotropy of the P and S wave in the four synthetic rocks shows that seismic anisotropy is directly proportional to increasing crack density, as predicted by several theoretical models. The laboratory measurements indicate that it would be effective to use seismic anisotropy to determine the crack density and estimate the intensity of crack density in seismology and seismic exploration.

  19. OPTICAL SPECTROSCOPIC OBSERVATIONS OF GAMMA-RAY BLAZAR CANDIDATES. V. TNG, KPNO, AND OAN OBSERVATIONS OF BLAZAR CANDIDATES OF UNCERTAIN TYPE IN THE NORTHERN HEMISPHERE

    Energy Technology Data Exchange (ETDEWEB)

    Álvarez Crespo, N.; Massaro, F. [Dipartimento di Fisica, Università degli Studi di Torino, via Pietro Giuria 1, I-10125 Torino (Italy); Masetti, N. [INAF—Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, I-40129, Bologna (Italy); Ricci, F.; La Franca, F. [Dipartimento di Matematica e Fisica, Università Roma Tre, via della Vasca Navale 84, I-00146, Roma (Italy); Landoni, M. [INAF-Osservatorio Astronomico di Brera, Via Emilio Bianchi 46, I-23807 Merate (Italy); Patiño-Álvarez, V.; Chavushyan, V.; Torrealba, J. [Instituto Nacional de Astrofisica, Óptica y Electrónica, Apartado Postal 51-216, 72000 Puebla, México (Mexico); D’Abrusco, R.; Paggi, A.; Smith, Howard A. [Harvard—Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 (United States); Jiménez-Bailón, E. [Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 877, Ensenada, 22800 Baja California, México (Mexico); Latronico, L. [Istituto Nazionale di Fisica Nucleare, Sezione di Torino, I-10125 Torino (Italy); Tosti, G. [Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia (Italy)

    2016-02-15

    The extragalactic γ-ray sky is dominated by emission from blazars, a peculiar class of active galactic nuclei. Many of the γ-ray sources included in the Fermi-Large Area Telescope Third Source catalog (3FGL) are classified as blazar candidates of uncertain type (BCUs) because there are no optical spectra available in the literature to confirm their nature. In 2013, we started a spectroscopic campaign to look for the optical counterparts of the BCUs and of the unidentified γ-ray sources to confirm their blazar nature. Whenever possible we also determine their redshifts. Here, we present the results of the observations carried out in the northern hemisphere in 2013 and 2014 at the Telescopio Nazionale Galileo, Kitt Peak National Observatory, and Observatorio Astronómico Nacional in San Pedro Mártir. In this paper, we describe the optical spectra of 25 sources. We confirmed that all of the 15 BCUs observed in our campaign and included in our sample are blazars and we estimated the redshifts for three of them. In addition, we present the spectra for three sources classified as BL Lacs in the literature but with no optical spectra available to date. We found that one of them is a quasar (QSO) at a redshift of z = 0.208 and the other two are BL Lacs. Moreover, we also present seven new spectra for known blazars listed in the Roma-BZCAT that have an uncertain redshift or are classified as BL Lac candidates. We found that one of them, 5BZB J0724+2621, is a “changing look” blazar. According to the spectrum available in the literature, it was classified as a BL Lac, but in our observation we clearly detected a broad emission line that led us to classify this source as a QSO at z = 1.17.

  20. OPTICAL SPECTROSCOPIC OBSERVATIONS OF GAMMA-RAY BLAZAR CANDIDATES. VI. FURTHER OBSERVATIONS FROM TNG, WHT, OAN, SOAR, AND MAGELLAN TELESCOPES

    Energy Technology Data Exchange (ETDEWEB)

    Álvarez Crespo, N.; Massaro, F. [Dipartimento di Fisica, Università degli Studi di Torino, via Pietro Giuria 1, I-10125 Torino (Italy); Milisavljevic, D.; Paggi, A.; Smith, Howard A. [Harvard—Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Landoni, M. [INAF-Osservatorio Astronomico di Brera, Via Emilio Bianchi 46, I-23807 Merate (Italy); Chavushyan, V.; Patiño-Álvarez, V. [Instituto Nacional de Astrofísica, Óptica y Electrónica, Apartado Postal 51-216, 72000 Puebla, México (Mexico); Masetti, N. [INAF—Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, I-40129, Bologna (Italy); Jiménez-Bailón, E. [Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 877, Ensenada, 22800 Baja California, México (Mexico); Strader, J.; Chomiuk, L. [Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 (United States); Katagiri, H.; Kagaya, M. [College of Science, Ibaraki University, 2-1-1, Bunkyo, Mito 310-8512 (Japan); Cheung, C. C. [Space Science Division, Naval Research Laboratory, Washington, DC 20375 (United States); D’Abrusco, R. [Department of Physical Sciences, University of Napoli Federico II, via Cinthia 9, I-80126 Napoli (Italy); Ricci, F.; La Franca, F. [Dipartimento di Matematica e Fisica, Università Roma Tre, via della Vasca Navale 84, I-00146, Roma (Italy); and others

    2016-04-15

    Blazars, one of the most extreme classes of active galaxies, constitute so far the largest known population of γ-ray sources, and their number is continuously growing in the Fermi catalogs. However, in the latest release of the Fermi catalog there is still a large fraction of sources that are classified as blazar candidates of uncertain type (BCUs) for which optical spectroscopic observations are necessary to confirm their nature and their associations. In addition, about one-third of the γ-ray point sources listed in the Third Fermi-LAT Source Catalog (3FGL) are still unassociated and lacking an assigned lower-energy counterpart. Since 2012 we have been carrying out an optical spectroscopic campaign to observe blazar candidates to confirm their nature. In this paper, the sixth of the series, we present optical spectroscopic observations for 30 γ-ray blazar candidates from different observing programs we carried out with the Telescopio Nazionale Galileo, William Herschel Telescope, Observatorio Astronómico Nacional, Southern Astrophysical Research Telescope, and Magellan Telescopes. We found that 21 out of 30 sources investigated are BL Lac objects, while the remaining targets are classified as flat-spectrum radio quasars showing the typical broad emission lines of normal quasi-stellar objects. We conclude that our selection of γ-ray blazar candidates based on their multifrequency properties continues to be a successful way to discover potential low-energy counterparts of the Fermi unidentified gamma-ray sources and to confirm the nature of BCUs.

  1. To Mercury dynamics

    Science.gov (United States)

    Barkin, Yu. V.; Ferrandiz, J. M.

    frequencies of free oscillations of core-mantle system of Mercury. Based on the mentioned data about Mercury (Barkin, 1976) we have been obtained the following model values of moments of inertia of the Mercury and for its core:A=0.3499534, B=0.3499667, C=0.35; A_c =B_c =0.1749767, C_c =0.175000 (1quad unit=mR^2, m and R is a mass and a mean radius of the Mercury). Here we used model values for moments of inertia of the core using also some analogy with axysimmetrical model of the core of the Moon from paper Williams et al. (2003). Corresponding periods of free oscillations were determined on the base specially constructed equations of developed theory. They are equal: T_1 =260543\\cdot Trot years and T_2 =0.999468\\cdot Trot (Trot =58.6462 days is a period of Mercury rotation). Last period determines long period of relative oscillation of the core and mantleT_r . The mentioned periods are equal: T_1 =713years and T_r =302years. Barkin's work was accepted by grant SAB2000-0235 of Ministry of Education of Spain and partially by grants AYA2001-0787 and ESP2001-4533 is also aknowledged. References Anderson J.D., Colombo G., Esposito P.B., Lau E.L., Trager G.B.: 1987. The mass, gravity field and ephemeris of Mercury. Icarus, pp. 337-349. Anselmi A., Scoon G.E.N.: 2001. BepiColombo, ESA's Mercury Cornerstone mission. Planetary and Space Science, 49, pp. 1409-1420. Barkin Yu.V.: 1976. About plane periodic motions of a rigid body in gravitational field of a sphere. Astron. J., v. 53, pp. 1110-1119. In Russian. Barkin Yu.V.: 1987. An analytical theory of the lunar rotational motion. Proc. Int. Symp. ``Figure and Dynamics of Earth, Moon and Planets'' (September 1986, Prague). Monograph series of VUGTK. Prague. Pp. 657-677. Beletskij V.V.: 1972. Resonance rotation of celestial bodies and Cassini's laws. Celestial Mechanics, v.6, N3, pp. 356-378. Colombo G.: 1966. Cassini's second and third laws, Astron. J., 71, p. 891. Esposito P.B., Anderson J.D., Ng A.T.Y.: 1977. Experimental

  2. Resonance dynamics and partial averaging in a restricted three-body system

    Science.gov (United States)

    Haghighipour, Nader

    2002-07-01

    Based on the value of the orbital eccentricity of an object and also its proximity to the exact resonant orbit in a three-body system, the pendulum approximation [S. F. Dermott and C. D. Murray, Nature (London) 319, 201 (1983)] or the second fundamental model of resonance [M. H. Andoyer, Bull. Astron. 20, 321 (1903); J. Henrard and A. Lemaître, Celest. Mech. 30, 197 (1983)] are commonly used to study the motion of that object near its resonant state. In this paper, we present the method of partial averaging as an analytical approach to study the dynamical evolution of a body near a resonance. To focus attention on the capabilities of this technique, a restricted, circular and planar three-body system is considered and the dynamics of its outer planet while captured in a resonance with the inner body is studied. It is shown that the first-order partially averaged system resembles a mathematical pendulum whose librational motion can be viewed as a geometrical interpretation of the resonance capture phenomenon. The driving force of this pendulum corresponds to the gravitational attraction of the inner body and its contribution, at different resonant states, is shown to be proportional to es, where s is the order of the resonance and e is the orbital eccentricity of the outer planet. As examples of such systems, the cases of (1:1), (1:2), and (1:3) resonances are discussed and the results are compared with known planetary systems such as the Sun-Jupiter-Trojan asteroids.

  3. Kronoseismology III: An update on Saturn-driven waves in the C ring

    Science.gov (United States)

    Nicholson, Philip D.; French, Richard G.; Hedman, Matthew M.

    2016-05-01

    In previous work (Hedman & Nicholson [2013] Astron. J. 146, 12; Ibid [2014] MNRAS 444, 1369; French et al. [2016] Icarus, in press) we have identified 9 inward-propagating density waves in Saturn's C ring with outer Lindblad resonances (OLRs) generated by internal oscillations in Saturn. The oscillations involved are sectoral f-modes (ie., fundamental modes with l = m) with m = 1, 2, 3, 4 and 10. In addition, 5 outward-propagating waves between radii of 84,800 and 86,600 km have been identified as density waves driven by 3:2 tesseral resonances with fixed gravitational anomalies within the planet. (See Hedman et al., this conference.)We have now examined additional C ring waves from the catalog of Baillie et al. [2011], in an attempt to identify several weaker and shorter-wavelength waves in the inner C ring. We use a modified version of our previous wavelet-based technique to coadd phase-corrected spectra from multiple occultations, using trial values of `m` and the pattern speed to predict their relative phases. This enables us to detect waves too weak to see in individual occultations. To date, 6 new waves have been identified. Two appear to be due to additional saturnian f-modes, with m = 2 and m = 9. The other 4 waves appear to be a new variety: outward-propagating bending waves driven at outer vertical resonances (OVRs) with Saturn internal oscillations with l = m + 1. We find waves with m = 4, 7, 8 & 9. All of the newly-identified waves are at radii less than 77,000 km and only the m = 4 OVR is near the location predicted by Marley & Porco [1993].

  4. Kronoseismology: An update on Saturnian waves in the C Ring

    Science.gov (United States)

    Nicholson, Philip D.; French, Richard G.; Hedman, Matthew M.; Cassini VIMS Team, Cassini RSS Team

    2016-10-01

    In previous work (Hedman & Nicholson [2013] Astron. J. 146, 12; Ibid [2014] MNRAS 444, 1369; French et al. [2016] Icarus, in press) we have identified 9 inward-propagating density waves in Saturn's middle C ring with resonances generated by internal oscillations in Saturn. The oscillations involved are sectoral f-modes (ie., fundamental modes with l = m) with m = 1, 2, 3, 4 and 10. In addition, 5 outward-propagating waves in the outer C ring have been identified as density waves driven by 3:2 resonances with fixed gravitational anomalies within the planet (see abstract by El Moutamid et al.)We have now examined several additional C ring waves from the catalog of Baillie et al. [2011], in an attempt to identify weaker and shorter-wavelength waves in the inner C ring. We use a modified version of our previous wavelet-based technique to co-add phase-corrected spectra from multiple occultations, using trial values of `m' and the pattern speed to predict their relative phases. This enables us to detect waves too weak to see in individual occultations. To date, 6 new waves have been identified. Two appear to be due to additional saturnian f-modes, but at unexpected locations. The other 4 waves appear to be a new variety: outward-propagating bending waves driven at vertical resonances with Saturn internal oscillations with l = m + 1. We find bending waves with m = 4, 7, 8 & 9. Only the m = 4 wave is near the location predicted by Marley & Porco [1993].

  5. VESPA: Developing the Planetary Science Virtual Observatory in H2020

    Science.gov (United States)

    Erard, S.; Cecconi, B.; Le Sidaner, P.; Capria, M. T.; Rossi, A. P.; Schmitt, B.; Andre, N.; Vandaele, A. C.; Scherf, M.; Hueso, R.; Maattanen, A. E.; Thuillot, W.; Achilleos, N.; Marmo, C.; Santolik, O.; Benson, K.

    2015-12-01

    In the frame of the Europlanet-RI program, a prototype Virtual Observatory dedicated to Planetary Science has been set up. Most of the activity was dedicated to the definition of standards to handle data in this field. The aim was to facilitate searches in big archives as well as sparse databases, to make on-line data access and visualization possible, and to allow small data providers to make their data available in an interoperable environment with minimum effort. This system makes intensive use of studies and developments led in Astronomy (IVOA), Solar Science (HELIO), and space archive services (IPDA). A general standard has been devised to handle the specific complexity of Planetary Science, e.g. in terms of measurement types and coordinate frames [1]. A procedure has been identified to install small data services, and several hands-on sessions have been organized already. A specific client (VESPA) has been developed at VO-Paris (http://vespa.obspm.fr), using a resolver for target names. Selected data can be sent to VO visualization tools such as TOPCAT or Aladin though the SAMP protocol. The Europlanet H2020 program started in Sept 2015 will provide support to new data services in Europe (30 to 50 expected), and focus on the improvement of the infrastructure. Future steps will include the development of a connection between the VO world and GIS tools, and integration of heliophysics, planetary plasma and reference spectroscopic data. The Europlanet H2020 project is funded by the European Commission under the H2020 Program, grant 654208. [1] Erard et al Astron & Comp 2014

  6. Structure coefficients for different initial metallicities for use in stellar analysis

    Science.gov (United States)

    Inlek, Gulay; Budding, Edwin; Demircan, Osman

    2017-09-01

    Internal structure coefficients for zero age Main Sequence (ZAMS) model stars with different initial metallicities are presented. A series of (Eggleton) stellar models with masses between 1-40 M_{⊙} and metallicities Z=0.0001, Z=0.001, Z=0.004, Z=0.01, Z=0.02, and Z=0.03 were used. We have also calculated the same coefficients for a recommended solar metallicity value Z=0.0134 (Asplund et al. in Annu. Rev. Astron. Astrophys. 47:481, 2009). For each model, values of the internal structure constants k2, k3, k4 and related coefficients have been derived by numerically integrating Radau's equation with the (FORTRAN) program RADAU. The (Eggleton) stellar models used come from the ` EZ-Web' compilation of the Dept. of Astronomy, University of Wisconsin, Madison. The calculations follow the procedure given by Inlek and Budding (Astrophys. Space Sci. 342:365, 2012). These new results were compared with others in the literature. We deduce that the current state of theoretical evaluation of structure coefficients is generally in sufficient agreement with data obtained from apsidal advance rates of selected well-observed eccentric eclipsing binary stars at the present time, given the probable errors of the latter. However, new results coming from more precise and extensive data sets in the wake of the Kepler Mission, or similar future surveys, may call for further theoretical specification or refinement. The derivation of structure coefficients from observations of apsidal motion in close eccentric binary systems requires specification of relevant parameters from light curve analysis. A self-consistent treatment then implies inclusion of the structure coefficients within the fitting function of such analysis.

  7. Tidal synchronization of close-in satellites and exoplanets: II. Spin dynamics and extension to Mercury and exoplanet host stars

    Science.gov (United States)

    Ferraz-Mello, Sylvio

    2015-08-01

    This paper deals with the application of the creep tide theory (Ferraz-Mello, Celest Mech Dyn Astron 116:109, 2013a) to the rotation of close-in satellites, Mercury, close-in exoplanets, and their host stars. The solutions show different behaviors with two extreme cases: close-in giant gaseous planets with fast relaxation (low viscosity) and satellites and Earth-like planets with slow relaxation (high viscosity). The rotation of close-in gaseous planets follows the classical Darwinian pattern: it is tidally driven toward a stationary solution that is synchronized with the orbital motion when the orbit is circular, but if the orbit is elliptical, it has a frequency larger than the orbital mean motion. The rotation of rocky bodies, however, may be driven to several attractors whose frequencies are times the mean motion. The number of attractors increases with the viscosity of the body and with the orbital eccentricity. The final stationary state depends on the initial conditions. The classical example is Mercury, whose rotational period is 2/3 of the orbital period (3/2 attractor). The planet behaves as a molten body with a relaxation that allowed it to cross the 2/1 attractor without being trapped but not to escape being trapped in the 3/2 one. In that case, the relaxation is estimated to lie in the interval (equivalent to a quality factor roughly constrained to the interval ). The stars have a relaxation similar to the hot Jupiters, and their rotation is also driven to the only stationary solution existing in these cases. However, solar-type stars may lose angular momentum due to stellar wind, braking the rotation and displacing the attractor toward larger periods. Old, active host stars with big close-in companions generally have rotational periods larger than the orbital periods of the companions. The paper also includes a study of energy dissipation and the evolution of orbital eccentricity.

  8. Solaris: a global network of autonomous observatories in the southern hemisphere

    Science.gov (United States)

    Kozłowski, S. K.; Sybilski, P.; Konacki, Maciej; Pawłaszek, R. K.; Ratajczak, Milena; Helminiak, K. G.

    2014-07-01

    We present Project Solaris, a network of four autonomous observatories in the Southern Hemisphere. The Project's primary goal is to detect and characterize circumbinary planets using the eclipse timing approach. This method requires high-cadence and long time-span photometric coverage of the binaries' eclipses, hence the observatories are located at sites having similar separation in longitude and nearly identical latitudes: South African Astronómical Observatory, Republic of South Africa (Solaris-1 and -2), Siding Spring Observatory, Australia (Solaris-3) and Complejo Astronomico El Leoncito, Argentina (Solaris-4). The headquarters coordinating and monitoring the network is based in Toruń, Poland. All four sites are operational as of December 2013. The instrument and hardware configurations are nearly identical. Each site is equipped with a 0.5-m Ritchey-Chrétien or Schmidt-Cassegrain optical tube assembly mounted on a direct-drive modified German equatorial mount along with a set of instruments. Computer, power and networking components are installed in rack cabinets. Everything is housed in sandwiched fiberglass clamshell 3.5-m diameter robotized domes. The Argentinian site is additionally equipped with a 20-ft office container. We discuss the design requirements of robotic observatories aimed to operate autonomously as a global network with concentration on efficiency, robustness and modularity. We also present a newly introduced spectroscopic mode of operation commissioned on the Solaris-1 telescope. Using a compact échelle spectrograph (20 000 resolution) mounted directly on the imaging train of the telescope, we are able to remotely acquire spectra. A fully robotic spectroscopic mode is planned for 2015.

  9. El núcleo de instituciones científicas matritenses en el Paseo del Prado desde el siglo XVIII

    Directory of Open Access Journals (Sweden)

    Baratas Díaz, Luis Alfredo

    1996-06-01

    Full Text Available Throughout second half of 18th century was constituted a scientific institutions centre around the “Paseo del Prado” (Royal Botanical Garden, Sciences Academy, Astronomic Observatory, General Hospital,.... The development of this scientific area suffered the vicissitudes and limitations that affected to the illustrated scientific policy. In 19th century the new educational and research centers establishment was scarce and laking of clear guidelines; the various projects to build a Sciences Faculty or the Arts and Trades School limited considerably the extension of the Royal Garden. In the first third of 20th century the constructing activity would be limited to the works in the Cajal Institute (plagued by misundestanding and upsetting and some constant remodeling works in the Velasco Museum and Royal Garden.

    A lo largo de la segunda mitad del siglo XVIII se constituyó en torno al actual Paseo del Prado un importante núcleo de instituciones científicas (Real Jardín Botánico, Academia de Ciencias, Observatorio Astronómico, Hospital General,.... El desarrollo de este foco científico sufrió las vicisitudes y limitaciones que afectaron a la política científica ilustrada. En el siglo XIX el establecimiento de nuevos centros docentes en esta zona fue escaso y carente de una idea directriz; los diversos proyectos para edificar una Facultad de Ciencias o la Escuela de Artes y Oficios limitaron considerablemente la extensión del Real Jardín. En el primer tercio del siglo XX la actividad constructora se limitaría a las obras en el Instituto Cajal (plagadas de malentendidos y desajustes y unas constantes obras de remodelación en el Museo Velasco y el Jardín Botánico.

  10. Application of time transfer function to McVittie spacetime: gravitational time delay and secular increase in astronomical unit

    Science.gov (United States)

    Arakida, Hideyoshi

    2011-08-01

    We attempt to calculate the gravitational time delay in a time-dependent gravitational field, especially in McVittie spacetime, which can be considered as the spacetime around a gravitating body such as the Sun, embedded in the FLRW (Friedmann-Lemaître-Robertson-Walker) cosmological background metric. To this end, we adopt the time transfer function method proposed by Le Poncin-Lafitte et al. (Class Quantum Gravity 21:4463, 2004) and Teyssandier and Le Poncin-Lafitte (Class Quantum Gravity 25:145020, 2008), which is originally related to Synge's world function Ω( x A , x B ) and enables to circumvent the integration of the null geodesic equation. We re-examine the global cosmological effect on light propagation in the solar system. The round-trip time of a light ray/signal is given by the functions of not only the spacial coordinates but also the emission time or reception time of light ray/signal, which characterize the time-dependency of solutions. We also apply the obtained results to the secular increase in the astronomical unit, reported by Krasinsky and Brumberg (Celest Mech Dyn Astron 90:267, 2004), and we show that the leading order terms of the time-dependent component due to cosmological expansion is 9 orders of magnitude smaller than the observed value of dAU/ dt, i.e., 15 ± 4 (m/century). Therefore, it is not possible to explain the secular increase in the astronomical unit in terms of cosmological expansion.

  11. Astrometric Solar-System Anomalies

    Science.gov (United States)

    Anderson, John D.

    2009-05-01

    There are four unexplained anomalies connected with astrometric data. Perhaps the most disturbing is the fact that when a spacecraft on a flyby trajectory approaches the Earth within 2000 km or less, it experiences a gain in total orbital energy per unit mass (Anderson et al., Phys. Rev. Lett. 100, 091102). This amounts to a net velocity increase of 13.5 mm/s for the NEAR spacecraft at a closest approach of 539 km, 3.9 mm/s for the Galileo spacecraft at 960 km, and 1.8 mm/s for the Rosetta spacecraft at 1956 km. Next, I suggest the change in the astronomical unit AU is definitely a concern. It is increasing by about 15 cm/yr (Krasinsky and Brumberg, Celes. Mech. & Dynam. Astron. 90, 267). The other two anomalies are perhaps less disturbing because of known sources of nongravitational acceleration. The first is an apparent slowing of the two Pioneer spacecraft as they exit the solar system in opposite directions (Anderson et al., Phys. Rev. D 65, 082004). Some, including me, are convinced this effect is of concern, but many are convinced it is produced by a nearly identical thermal emission from both spacecraft, in a direction away from the Sun, thereby producing acceleration toward the Sun. The fourth anomaly is a measured increase in the eccentricity of the Moon's orbit. Here again, an increase is expected from tidal friction in both the Earth and Moon. However, there is a reported increase that is about three times larger than expected (J. G. Williams, DDA/AAS Brouwer Award Lecture, Halifax, Nova Scotia 2006). We suspect that all four anomalies have mundane explanations. However, the possibility that they will be explained by a new theory of gravitation is not ruled out, perhaps analogous to Einstein's 1916 explanation of the excess precession of Mercury's perihelion.

  12. A 3D tomographic reconstruction method to analyze Jupiter's electron-belt emission observations

    Science.gov (United States)

    Santos-Costa, Daniel; Girard, Julien; Tasse, Cyril; Zarka, Philippe; Kita, Hajime; Tsuchiya, Fuminori; Misawa, Hiroaki; Clark, George; Bagenal, Fran; Imai, Masafumi; Becker, Heidi N.; Janssen, Michael A.; Bolton, Scott J.; Levin, Steve M.; Connerney, John E. P.

    2017-04-01

    Multi-dimensional reconstruction techniques of Jupiter's synchrotron radiation from radio-interferometric observations were first developed by Sault et al. [Astron. Astrophys., 324, 1190-1196, 1997]. The tomographic-like technique introduced 20 years ago had permitted the first 3-dimensional mapping of the brightness distribution around the planet. This technique has demonstrated the advantage to be weakly dependent on planetary field models. It also does not require any knowledge on the energy and spatial distributions of the radiating electrons. On the downside, it is assumed that the volume emissivity of any punctual point source around the planet is isotropic. This assumption becomes incorrect when mapping the brightness distribution for non-equatorial point sources or any point sources from Juno's perspective. In this paper, we present our modeling effort to bypass the isotropy issue. Our approach is to use radio-interferometric observations and determine the 3-D brightness distribution in a cylindrical coordinate system. For each set (z, r), we constrain the longitudinal distribution with a Fourier series and the anisotropy is addressed with a simple periodic function when possible. We develop this new method over a wide range of frequencies using past VLA and LOFAR observations of Jupiter. We plan to test this reconstruction method with observations of Jupiter that are currently being carried out with LOFAR and GMRT in support to the Juno mission. We describe how this new 3D tomographic reconstruction method provides new model constraints on the energy and spatial distributions of Jupiter's ultra-relativistic electrons close to the planet and be used to interpret Juno MWR observations of Jupiter's electron-belt emission and assist in evaluating the background noise from the radiation environment in the atmospheric measurements.

  13. CALIFA, the Calar Alto Legacy Integral Field Area survey. II. First public data release

    Science.gov (United States)

    Husemann, B.; Jahnke, K.; Sánchez, S. F.; Barrado, D.; Bekerait*error*ė, S.; Bomans, D. J.; Castillo-Morales, A.; Catalán-Torrecilla, C.; Cid Fernandes, R.; Falcón-Barroso, J.; García-Benito, R.; González Delgado, R. M.; Iglesias-Páramo, J.; Johnson, B. D.; Kupko, D.; López-Fernandez, R.; Lyubenova, M.; Marino, R. A.; Mast, D.; Miskolczi, A.; Monreal-Ibero, A.; Gil de Paz, A.; Pérez, E.; Pérez, I.; Rosales-Ortega, F. F.; Ruiz-Lara, T.; Schilling, U.; van de Ven, G.; Walcher, J.; Alves, J.; de Amorim, A. L.; Backsmann, N.; Barrera-Ballesteros, J. K.; Bland-Hawthorn, J.; Cortijo, C.; Dettmar, R.-J.; Demleitner, M.; Díaz, A. I.; Enke, H.; Florido, E.; Flores, H.; Galbany, L.; Gallazzi, A.; García-Lorenzo, B.; Gomes, J. M.; Gruel, N.; Haines, T.; Holmes, L.; Jungwiert, B.; Kalinova, V.; Kehrig, C.; Kennicutt, R. C.; Klar, J.; Lehnert, M. D.; López-Sánchez, Á. R.; de Lorenzo-Cáceres, A.; Mármol-Queraltó, E.; Márquez, I.; Mendez-Abreu, J.; Mollá, M.; del Olmo, A.; Meidt, S. E.; Papaderos, P.; Puschnig, J.; Quirrenbach, A.; Roth, M. M.; Sánchez-Blázquez, P.; Spekkens, K.; Singh, R.; Stanishev, V.; Trager, S. C.; Vilchez, J. M.; Wild, V.; Wisotzki, L.; Zibetti, S.; Ziegler, B.

    2013-01-01

    We present the first public data release (DR1) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. It consists of science-grade optical datacubes for the first 100 of eventually 600 nearby (0.005 characteristics and data structure of the CALIFA datasets that should be taken into account for scientific exploitation of the data, in particular the effects of vignetting, bad pixels and spatially correlated noise. The data quality test for all 100 galaxies showed that we reach a median limiting continuum sensitivity of 1.0 × 10-18 erg s-1 cm-2 Å-1 arcsec-2 at 5635 Å and 2.2 × 10-18 erg s-1 cm-2 Å-1 arcsec-2 at 4500 Å for the V500 and V1200 setup respectively, which corresponds to limiting r and g band surface brightnesses of 23.6 mag arcsec-2 and 23.4 mag arcsec-2, or an unresolved emission-line flux detection limit of roughly 1 × 10-17 erg s-1 cm-2 arcsec-2 and 0.6 × 10-17 erg s-1 cm-2 arcsec-2, respectively. The median spatial resolution is 3farcs7, and the absolute spectrophotometric calibration is better than 15% (1σ). We also describe the available interfaces and tools that allow easy access to this first publicCALIFA data at http://califa.caha.es/DR1 Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max- Planck-Institut für Astronomie (MPIA) and the Instituto de Astrofísica de Andalucía (CSIC).

  14. Reconstructing the dark sector interaction with LISA

    Science.gov (United States)

    Cai, Rong-Gen; Tamanini, Nicola; Yang, Tao

    2017-05-01

    We perform a forecast analysis of the ability of the LISA space-based interferometer to reconstruct the dark sector interaction using gravitational wave standard sirens at high redshift. We employ Gaussian process methods to reconstruct the distance-redshift relation in a model independent way. We adopt simulated catalogues of standard sirens given by merging massive black hole binaries visible by LISA, with an electromagnetic counterpart detectable by future telescopes. The catalogues are based on three different astrophysical scenarios for the evolution of massive black hole mergers based on the semi-analytic model of E. Barausse, Mon. Not. Roy. Astron. Soc. 423 (2012) 2533. We first use these standard siren datasets to assess the potential of LISA in reconstructing a possible interaction between vacuum dark energy and dark matter. Then we combine the LISA cosmological data with supernovae data simulated for the Dark Energy Survey. We consider two scenarios distinguished by the time duration of the LISA mission: 5 and 10 years. Using only LISA standard siren data, the dark sector interaction can be well reconstructed from redshift z~1 to z~3 (for a 5 years mission) and z~1 up to z~5 (for a 10 years mission), though the reconstruction is inefficient at lower redshift. When combined with the DES datasets, the interaction is well reconstructed in the whole redshift region from 0z~ to z~3 (5 yr) and z~0 to z~5 (10 yr), respectively. Massive black hole binary standard sirens can thus be used to constrain the dark sector interaction at redshift ranges not reachable by usual supernovae datasets which probe only the zlesssim 1.5 range. Gravitational wave standard sirens will not only constitute a complementary and alternative way, with respect to familiar electromagnetic observations, to probe the cosmic expansion, but will also provide new tests to constrain possible deviations from the standard ΛCDM dynamics, especially at high redshift.

  15. Geotechnical Study of the OAN/SPM

    Science.gov (United States)

    Sánchez, B.; Castellanos, V.; Castilla, J. E.; Grijalva, J.; Díaz v., G.; Porres, R.; Garay, F.; Zamarripa, V.

    2003-09-01

    The geotechnical characterization of the San Pedro Mártir (SPM), Baja California site was carried out in 2000 by the Gerencia de Estudios de Ingeniería Civil of the Comisión Federal de Electricidad (GEIC/CFE). The principal aim of the series of geological and geotechnical studies was to characterize the subsoil performance at one of the possible construction sites of a new telescope, which may also provide an idea of the characteristics of other locations at the Observatorio Astronómico Nacional in San Pedro Mártir (OAN/SPM) Sierra summit. The full report of the GEIC/CFE geotechnical study of the SPM site includes results from the topographic, geological and geophysical surveys carried out. In the present paper a review of the geotechnical study is presented and some of the important results are summarized. The study shows that the subsoil can be classified in three principal horizons or layers (A, B and C). The A-horizon consists of decompressed rock of depth 1.3 to 3.0 m, which has to be removed for the foundations. Layer B consists of fractured rock with an RQD (rock quality designation) between 65%-80%, a thickness of 10-12 m, and a high load bearing capacity. This implies that the required depth excavations for the foundation footings ranges from 2 to 3 m, where an adequate dynamic modulus of elasticity can be reached. Horizon C from 13 to 22 m, the maximum depth explored, consists of rock (gray schist) of massive nature with some granite intrusions that appears slightly fractured, with an RQD above 90%. For the electric grounding instalation the best place is layer B due to its lower resistivity.

  16. A New Look at Photometry of the Moon

    Science.gov (United States)

    Goguen, Jay D.; Stone, T. C.; Kieffer, H. H.; Buratti, B. J.

    2010-10-01

    We test 2 very different models for light scattering by the lunar regolith: 1) TRLA - a Topographically Rough surface layer comprised of Low Albedo particles, and 2) RTE - a flat surface layer with the published size distribution and optical constants of Apollo soil particles, Mie calculation of the mean particle scattering matrix and rigorous solution of the Radiative Transfer Equation for all orders of scattering (Mishchenko et al 1999, JQRST 63, 409). For a typical lunar highland location (-17.21, 20.01), ROLO photometry (Kieffer & Stone 2005, Astron. J. 129, 2887) shows a distinct difference between the radiances measured before and after full moon (BFM, AFM) at the same 47.5 ± 2.5 degree phase angle, corresponding to incidence angles of 30 and 70 degrees, respectively. The TRLA model requires rms slopes of 34.1 ± 2.6 degrees to reproduce this BFM/AFM radiance difference, similar to previously published results. Analysis of Apollo ALSCC stereo images of in situ lunar regolith (Helfenstein and Shepard 1999, Icarus 141, 107) shows that such large rms slopes pertain to a sub-mm horizontal distance scale. The RTE model also reproduces the same BFM/AFM radiance difference, but as a direct consequence of multiple scattering between particles within the flat (zero topographic roughness) regolith layer. Approximately 80% of the radiance in the RTE model is contributed by photons scattered more than once. We conclude that topographic roughness of the regolith surface and multiple scattering between regolith particles can have a nearly identical effect on this BFM/AFM difference in the lunar radiance. Roughness and multiple scattering are strongly correlated parameters in the sense that any approximations regarding one of them will influence the value deduced for the other. A complete treatment of this work is published in Goguen et al 2010, Icarus 208, 548.

  17. ANÁLISE DAS CONCEPÇÕES ASTRONÔMICAS APRESENTADAS POR PROFESSORES DE CIÊNCIAS, FÍSICA E MATEMÁTICA DA REDE MUNICIPAL DE SÃO JOSÉ DOS CAMPOS / SP

    Directory of Open Access Journals (Sweden)

    Edson Pereira Gonzaga

    2013-12-01

    Full Text Available Pretende-se, aqui, realizar o levantamento das concepções alternativas acerca dos conceitos básicosda Astronomia, junto aos professores da rede municipal de ensino de São José dos Campos, podendo seestender à rede estadual de ensino e estando em conformidade com documentos legais relacionados aocurrículo das redes de ensino, como O Currículo do Estado de São Paulo e os Parâmetros CurricularesNacionais (PCNs. A ideia de concepções alternativas mencionadas por Langhi (2009 será de extremaimportância, pois acredita-se que, se for possível saber tais concepções antes da intervenção metodológica, serápossível preparar apresentações contextualizadas e propor que os professores relacionem o que sabem com asinformações apresentadas nas sessões de planetário móvel da Universidade Cruzeiro do Sul e, posteriormente,que possam discutir em um fórum de discussões, sob forma de debate, procurando estabelecer conclusõespertinentes ao tema e sua transmissão para estudantes da Educação Básica (EB. Trata-se de um estudo decaso com intervenção metodológica, levantamento quantitativo e análise qualitativa dos dados, sobre osconceitos astronômicos por meio de dois questionários, um antes e outro depois da intervenção, respeitando operíodo de aplicação do estudo, chama-se, aqui, de intervenção metodológica as apresentações de conteúdo noplanetário móvel e as respectivas discussões.

  18. An analysis of the convergence of Newton iterations for solving elliptic Kepler's equation

    Science.gov (United States)

    Elipe, A.; Montijano, J. I.; Rández, L.; Calvo, M.

    2017-12-01

    In this note a study of the convergence properties of some starters E_0 = E_0(e,M) in the eccentricity-mean anomaly variables for solving the elliptic Kepler's equation (KE) by Newton's method is presented. By using a Wang Xinghua's theorem (Xinghua in Math Comput 68(225):169-186, 1999) on best possible error bounds in the solution of nonlinear equations by Newton's method, we obtain for each starter E_0(e,M) a set of values (e,M) \\in [0, 1) × [0, π ] that lead to the q-convergence in the sense that Newton's sequence (E_n)_{n ≥ 0} generated from E_0 = E_0(e,M) is well defined, converges to the exact solution E^* = E^*(e,M) of KE and further \\vert E_n - E^* \\vert ≤ q^{2^n -1} \\vert E_0 - E^* \\vert holds for all n ≥ 0. This study completes in some sense the results derived by Avendaño et al. (Celest Mech Dyn Astron 119:27-44, 2014) by using Smale's α -test with q=1/2. Also since in KE the convergence rate of Newton's method tends to zero as e → 0, we show that the error estimates given in the Wang Xinghua's theorem for KE can also be used to determine sets of q-convergence with q = e^k \\widetilde{q} for all e \\in [0,1) and a fixed \\widetilde{q} ≤ 1. Some remarks on the use of this theorem to derive a priori estimates of the error \\vert E_n - E^* \\vert after n Kepler's iterations are given. Finally, a posteriori bounds of this error that can be used to a dynamical estimation of the error are also obtained.

  19. Acetylene ^1^2C_2H_2 Laboratory Measurements for Astrophysical Applications

    Science.gov (United States)

    Jacquemart, D.; Gomez, L.; Lacome, N.; Mandin, J.-Y.; Pirali, O.; Roy, P.

    2010-06-01

    The acetylene molecule is important for atmospheric, planetary, and astrophysical applications. This organic molecule, known as a precursor of amino acids, shows numerous vibration-rotation bands in the IR. Two recent works on line intensities measurements will be presented. A study around 7.7 μm was motivated by SPITZER observations of C_2H_2 in this spectral region that cannot be modeled using the current line list of HITRAN/GEISA due to the lack of data. High resolution spectra have been recorded with the Bruker HR IFS 120 of the LADIR and analyzed to deduce absolute line intensities of several bands included the one present in HITRAN, the (ν_4+ν_5)^0_+ strong band. On the whole, line intensities of 2 cold bands and 15 hot bands have been studied, and a complete line list has been generated. Another study using SOLEIL synchrotron will be presented in the spectral region around 100 cm^-^1 of interest for astrophysical applications (SPITZER, ALMA, HERSCHEL...). High resolution spectra have been recorded with the Bruker HR IFS 125 of SOLEIL. For accurate line intensities measurement based on the FIR beam of the synchrotron, the strong wavenumber dependence of the beam radius had to be modeled in the apparatus function calculation. Absolute line intensities of the intense ν_5-ν_4 band have been measured, and those of the 4 weaker hot bands are in progress. M. Matzuura et al. Non. Not. R. Astron. Soc. 371, 415-420, 2006. J. Vander Auwera. J. Mol. Spectrosc. 242, 25-30, 2007. L. Gomez, D. Jacquemart, N. Lacome and J.-Y. Mandin. JQSRT 110, 2102-2114, 2009. D. Jacquemart, L. Gomez, N. Lacome, J.-Y. Mandin, O. Pirali and P. Roy. JQSRT in press.

  20. Situação da Mulher na Astronomia Brasileira

    Science.gov (United States)

    Silva, Adriana V. R.

    2007-07-01

    O conteúdo desse texto surgiu de uma apresentação de mesmo título que fiz na XXXI Reunião Anual da Sociedade Astronômica Brasileira (SAB) em 2005. Esse tema foi inspirado originalmente pela minha participação no "2nd UIPAP International Conference on Women in Physics" realizado entre 23 e 25 de maio de 2005 no Rio de Janeiro. Essa é uma conferência internacional que acontece de três em três anos, sendo que a primeira ocorreu em 2002 na cidade de Paris, França. Participei dessa conferência como membro da delegação da Sociedade Brasileira de Física e um dos trabalhos que apresentei versava sobre a situação das mulheres na Astronomia brasileira, cujos resultados principais discorro a seguir. A situação das astrônomas, baseada nos dados dos sócios da SAB coletados no final de 2004, é comparada com a das físicas brasileiras e também com as nossas colegas americanas. Os dados identificam ainda uma maior evasão da carreira por parte das mulheres do que os homens. Alguns dos possíveis motivos da evasão são discutidos, como o desejo de constituir família e/ou isolamento. Resultados um tanto preocupantes com relação à distribuição de bolsas de produtividade do CNPq também são apresentados. As principais discussões e estratégias recomendadas nesse congresso são mencionadas de forma resumida ao final.

  1. Museo Arqueológico de Petroglifos y el fomento del turismo en Venezuela

    Directory of Open Access Journals (Sweden)

    Yamile Delgado De Smith

    2005-11-01

    Full Text Available El Complejo Arqueológico de Vigirima (Venezuela es el mayor yacimiento de Petroglifos de América y el único lugar continental que presenta alineamientos megalíticos. Sin embargo, es poco conocido y ha sido aún menos estudiado, quedando a la saga de los proyectos de conservación y preservación patrimonial emprendidos por los organismos supranacionales. Se efectuó un registro sistemático y la clasificación estilística de los glifos y caracteres pétreos del complejo arqueológico de Vigirima. El análisis de las técnicas de elaboración, del substrato y su distribución espacio temporal muestran que los mismos fueron elaborados con diversos grados de especificidad por los grupos humanos que crearon estas expresiones de arte rupestre. Los contenidos y estilos informan sobre una sociedad en estrecha dependencia y en equilibrio frente a la naturaleza, en cuya organización tribal, de carácter igualitario, tendría un rol importante: el Chaman como mediador hombre-naturaleza y la mujer como símbolo de la reproducción de la fuerza humana de trabajo. Se presentan, adicionalmente, elementos contextuales que permiten datar la antigüedad del yacimiento y las tradiciones míticas de carácter mágico-religioso o astronómico, que pudieron motivarlo y finalmente se proponen alternativas para su conservación y el fomento del turismo.

  2. Health promotion, preventive and curative aspects of diseases in astrology.

    Science.gov (United States)

    Sharma, Bhuvnesh Kumar; Subhakta, P K J P; Narayana, A

    2007-01-01

    The whole universe is intermingling into a unit in the period of globalization. Different cultures, life-styles and sciences are co-operating with each other in this situation. World Health Organization is working towards collaborating all prevalent medical sciences for attainment of good health and family welfare for each and every individual by 2020. Astrology is a part of Indian heritage. Astrology means the art of predicting or determining the influence of the planets and stars on human affairs. The origin of this word is from Greek word astron, star + logos (discourse). The account of deeds of good and bad during the present life and previous lives, their consequences of health or ill health during this life i.e. what, when and how the things takes place will be clearly known through Astrology. Highly advanced knowledge related to Astrology on medicine is preserved in Indian scriptures and the knowledge was transmitted from generation to generation. It is also a good source for health promotion, preventive, curative and other medical aspects. Brief direction related to astrological medical aspects is also available in Ayurvedic literature (Carakasamhită, Suśrutasamhhită, Aşţăngasangraha, Aşţăngahŗdaya, Sărngadharasamhită , Băvaprakăśa etc.) Some Ayurvedic practitioners, scholars and scientists realize the need of astrological knowledge related to medicine in the present time. In ancient times physician, astrologer and purŏhita (Hindu priest) simultaneously looked after the health and family welfare of individual, families and country. Astrologer guides medication and suitable time for the better cure of ailments. Even the medicinal herbs were collected and treated at appropriate time for their efficacy. Astrology and Ayurvĕda are inseparable sciences of life. Hence, in this article, a concise astrological evaluation related to health promotion, preventive and curative aspects of Astrology is being presented.

  3. Contribution of astrology in medicine -- a review.

    Science.gov (United States)

    Sharma, Bhuvnesh Kumar; Prasad, P V V; Narayana, A

    2007-01-01

    Astrology is the art of predicting or determining the influence of the planets and stars on human affairs. The origin of this word is from Greek word astron, star + logos (discourse). Both Ayurveda and Astrology have established a way of life in India since time immemorial. Highly advanced knowledge related to Astrology on medicine is preserved in Indian Holy scriptures and transmitted from generation to generation. Although both Astrology and medicine were developed as a part of religion in ancient India, astrological principles related to prevention, health care and relief from illness were applied as rituals (religious ceremonies). An astrologer gives guidance for taking medicines at suitable time for the best remedy of ailments. Even the medicinal herbs were collected and used at appropriate times for their efficacy. Astrology and Ayurveda are inseparable in human life. Role of the Astrology in healthy life and pathogenesis of the disease is well known to Indians. When a physician knows etiology of the disease, he attempts to treat the disease with specific medication, diet and life style and also avoiding causative factors. In a case where a physician is unable to understand the pathogenesis of the disease and to treat, the patient depends upon Astrology. Account of good and bad deeds during this life and previous lives, their consequences of health or ill health during this life which orderly, when, what and how will be clearly known through Astrology. It gives guidelines about welfare not only to human being but also to whole creation and also indicates about calamities and their solutions as possible extent. Hence a concise astrological evaluation related to prevention, health care, diagnosis and treatment of diseases is being presented in this article.

  4. Integrated spectral study of small angular diameter galactic open clusters

    Science.gov (United States)

    Clariá, J. J.; Ahumada, A. V.; Bica, E.; Pavani, D. B.; Parisi, M. C.

    2017-10-01

    This paper presents flux-calibrated integrated spectra obtained at Complejo Astronómico El Leoncito (CASLEO, Argentina) for a sample of 9 Galactic open clusters of small angular diameter. The spectra cover the optical range (3800-6800 Å), with a resolution of ∼14 Å. With one exception (Ruprecht 158), the selected clusters are projected into the fourth Galactic quadrant (282o age by comparing the continuum distribution and line strenghts of the cluster spectra with those of template cluster spectra with known parameters. We thus provide spectroscopic information independent from that derived through color-magnitude diagram studies. We found three clusters (Collinder 249, NGC 4463 and Ruprecht 122) younger than ∼40 Myr, four moderately young ones (BH 92, Harvard 5, Hogg 14 and Pismis 23) with ages within 200-400 Myr, and two intermediate-age ones (Ruprecht 158 and ESO 065-SC07) with ages within 1.0-2.2 Gyr. The derived foreground E(B - V) color excesses vary from around 0.0 in Ruprecht 158 to ∼1.1 in Pismis 23. In general terms, the results obtained show good agreement with previous photometric results. In Ruprecht 158 and BH 92, however, some differences are found between the parameters here obtained and previous values in the literature. Individual spectra of some comparatively bright stars located in the fields of 5 out of the 9 clusters here studied, allowed us to evaluate their membership status. The current cluster sample complements that of 46 open clusters previously studied by our group in an effort to gather a spectral library with several clusters per age bin. The cluster spectral library that we have been building is an important tool to tie studies of resolved and unresolved stellar content.

  5. The effects of the WISE/ GALEX photometry for the SED-fitting with M31 star clusters and candidates

    Science.gov (United States)

    Fan, Zhou; Wang, Song

    2017-10-01

    Spectral energy distribution (SED) fitting of stellar population synthesis models is an important and popular way to constrain the physical parameters—e.g., the ages, metallicities, masses for stellar population analysis. The previous works suggest that both blue-bands and red-bands photometry works for the SED-fitting. Either blue-domained or red-domained SED-fitting usually lead to the unreliable or biased results. Meanwhile, it seems that extending the wavelength coverage could be helpful. Since the Galaxy Evolution Explorer ( GALEX) and Wide-field Infrared Survey Explorer (WISE) provide the FUV/NUV and mid-infrared W1/W2 band data, we extend the SED-fitting to a wider wavelength coverage. In our work, we analyzed the effect of adding the FUV/NUV and W1/W2 band to the optical and near-infrared UBVRIJHK bands for the fitting with the (Bruzual and Charlot in Mon. Not. R. Astron. Soc. 344, 1000, 2003) (BC03) models and galev models. It is found that the FUV/NUV bands data affect the fitting results of both ages and metallicities much more significantly than that of the WISE W1/W2 band with the BC03 models. While for the galev models, the effect of the WISE W1/W2 band for the metallicity fitting seems comparable to that of GALEX FUV/NUV bands, but for age the effect of the W1/W2 band seems less crucial than that of the FUV/NUV bands. Thus we conclude that the GALEX FUV/NUV bands are more crucial for the SED-fitting of ages and metallicities, than the other bands, and the high-quality UV data (with high photometry precision) are required.

  6. High Resolution Measurements and Electronic Structure Calculations of a Diazanaphthalene

    Science.gov (United States)

    Gruet, Sébastien; Goubet, Manuel; Pirali, Olivier

    2014-06-01

    Polycyclic Aromatic Hydrocarbons (PAHs) have long been suspected to be the carriers of so called Unidentified Infrared Bands (UIBs). Most of the results published in the literature report rotationally unresolved spectra of pure carbon as well as heteroatom-containing PAHs species. To date for this class of molecules, the principal source of rotational informations is ruled by microwave (MW) spectroscopy while high resolution measurements reporting rotational structure of the infrared (IR) vibrational bands are very scarce. Recently, some high resolution techniques provided interesting new results to rotationally resolve the IR and far-IR bands of these large carbonated molecules of astrophysical interest. One of them is to use the bright synchrotron radiation as IR continuum source of a high resolution Fourier transform (FTIR) spectrometer. We report the very complementary analysis of the [1,6] naphthyridine (a N-bearing PAH) for which we recorded the microwave spectrum at the PhLAM laboratory (Lille) and the high resolution far-infrared spectrum on the AILES beamline at synchrotron facility SOLEIL. MW spectroscopy provided highly accurate rotational constants in the ground state to perform Ground State Combinations Differences (GSCD) allowing the analysis of the two most intense FT-FIR bands in the 50-900 wn range. Moreover, during this presentation the negative value of the inertial defect in the GS of the molecule will be discussed. A. Leger, J. L. Puget, Astron. Astrophys. 137, L5-L8 (1984) L. J. Allamandola et al. Astrophys. J. 290, L25-L28 (1985). Z. Kisiel et al. J. Mol. Spectrosc. 217, 115 (2003) S. Thorwirth et al. Astrophys. J. 662, 1309 (2007) D. McNaughton et al. J. Chem. Phys. 124, 154305 (2011). S. Albert et al. Faraday Discuss. 150, 71-99 (2011) B. E. Brumfield et al. Phys. Chem. Lett. 3, 1985-1988 (2012) O. Pirali et al. Phys. Chem. Chem. Phys. 15, 10141 (2013).

  7. Astronomy Teaching in Argentina in the 19th Century. (Spanish Title: La Enseñanza de la Astronomía en la Argentina del Siglo XIX.) O Ensino de Astronomia na Argentina no Século XIX

    Science.gov (United States)

    Norberto Cornejo, Jorge; Santilli, Haydée

    2010-12-01

    Sarmiento believed that Copernican astronomy was one of the critical scientific disciplines to the formation of a "modern" citizen. In this work, we shall study astronomical science from two points of view: from the scientific knowledge and the educational presentation of such knowledge. Our study will address in Argentina in 19th century, starting from the initiative of Bernardino Rivadavia in 1821, who founded an astronomic observatory at Buenos Aires, until the first activities of the observatories at Córdoba and La Plata. On both lines, scientific and educative, we shall analyze the influence of positivist ideas. We shall highlight epistemological differences between both observatories, Córdoba's based on French positivism and La Plata's based on German positivism. We shall also show the different attitude of both observatories towards education. We shall see the way in which positivist ideas had great relevance in the training of elementary school teachers. We shall also establish the relevant influence of the socio-historical context over the astronomical development, and show that astronomy was a fundamental social factor at Argentina history. Domingo F. Sarmiento consideraba que la astronomía copernicana era una de las disciplinas científicas fundamentales para la conformación de un ciudadano "moderno". En este trabajo estudiaremos la ciencia astronómica desde dos vertientes: la referida específicamente al conocimiento científico y aquella vinculada con la presentación educativa de dicho conocimiento. Nuestro estudio se desarrollará en Argentina durante el siglo XIX, desde la iniciativa de Bernardino Rivadavia en 1821, de establecer en Buenos Aires un observatorio astronómico, hasta las primeras actividades de los observatorios de Córdoba y de La Plata. En ambas vertientes, científica y educativa, analizaremos la influencia de las ideas positivistas. Resaltaremos las diferencias epistemológicas entre los dos observatorios, orientado el primero

  8. Evolution of the Astronomy Concepts Along Basic Education Cycle. (Breton Title: Evolução dos Conceitos de Astronomia no Decorrer da Educação Básica.) La Evolución de los Conceptos de Astronomía Durante la Educación Básica

    Science.gov (United States)

    Darroz, Luiz Marcelo; da Rosa, Cleci Werner; Becker da Rosa, Álvaro; Samudio Pèrez, Carlos Ariel

    2014-07-01

    learning of astronomy in basic education. Embora a astronomia seja considerada uma das ciências mais antigas da humanidade e ainda que a compreensão de seus conceitos tenha trazido enormes avanços para a Ciência e, consequentemente, para a sociedade, observa-se que uma parcela significativa de pessoas encontra-se à margem desses conhecimentos. De acordo com os Parâmetros Curriculares Nacionais para a Educação Básica, cabe à escola a difusão dos conceitos cientificamente corretos, entre eles os relacionados à área de astronomia. Pertinente a essa questão, apresenta-se uma pesquisa realizada com 140 estudantes do nono ano do ensino fundamental e com 120 estudantes da terceira série do ensino médio de quatro escolas da região de Passo Fundo/RS. Buscou-se averiguar, por meio de um questionário composto de questões abertas e de múltipla escolha, o conhecimento desse grupo de estudantes acerca de termos e fenômenos astronômicos básicos e, também, verificar se o índice de acertos cresce à medida que eles avançam nas diferentes e gradativas séries dos ensinos fundamental e médio. De modo geral, os resultados apresentados demonstram que o ensino de astronomia na educação básica enfrenta deficiências. Das 20 questões investigadas, em 17 os índices de acertos são semelhantes nas respostas dadas por estudantes de nível fundamental e médio, revelando que muitas concepções equivocadas permanecem ao longo da educação básica. Isso evidencia que tais temas não são - ou são pouco - abordados durante esses dois níveis de escolarização. Assim, conclui-se que a discussão dos conceitos relacionados com a astronomia deve receber maior ênfase na abordagem dos diferentes conteúdos, sendo necessária uma ação nacional em prol do seu ensino. Acredita-se que essa ação nacional deve estar apoiada em um pilar triplo de atores coletivos: comunidade científica, comunidade astronômica semiprofissional e comunidade escolar. Por fim, esse pilar seria

  9. The Binary Fission Model for the Formation of the Pluto system

    Science.gov (United States)

    Prentice, Andrew

    2016-10-01

    The ratio F of the mass of Pluto (P) to Charon (C), viz. F ≈ 8:1, is the largest ratio of any planet-satellite pair in the solar system. Another measure of the PC binary is its normalized angular momentum density J (see McKinnon 1989). Analysis of astrometric data (Brozovic et al 2015) acquired before the New Horizons (NH) arrival at Pluto and new measurements made by NH (Stern et al 2015) show that J = 0.39. Yet these F & J values are ones expected if the PC binary had formed by the rotational fission of a single liquid mass (Darwin 1902; Lyttleton 1953). At first glance, therefore, the fission model seems to be a viable model for the formation of the Pluto system. In fact, Prentice (1993 Aust J Astron 5 111) had used this model to successfully predict the existence of several moons orbiting beyond Charon, before their discovery in 2005-2012. The main problem with the fission model is that the observed mean density of Charon, namely 1.70 g/cm3, greatly exceeds that of water ice. Charon thus could not have once been a globe of pure water. Here I review the fission model within the framework of the modern Laplacian theory of solar system origin (Prentice 1978 Moon Planets 19 341; 2006 PASA 23 1) and the NH results. I assume that Pluto and Charon were initially a single object (proto-Pluto [p-P]) which had condensed within the same gas ring shed by the proto-solar cloud at orbital distance ~43 AU, where the Kuiper belt was born. The temperature of this gas ring is 26 K and the mean orbit pressure is 1.3 × 10-9 bar. After the gas ring is shed, chemical condensation takes place. The bulk chemical composition of the condensate is anhydrous rock (mass fraction 0.5255), graphite (0.0163), water ice (0.1858), CO2 ice (0.2211) and methane ice (0.0513). Next I assume that melting of the ices in p-P takes place through the decay of short-lived radioactive nuclides, thus causing internal segregation of the rock & graphite. Settling of heavy grains to the centre lowers the

  10. Projeto educação em ciências com observatórios virtuais: a participação da Escola Moppe no período 2000-2003

    Science.gov (United States)

    Wuensche, C. A.; Gavioli, E.; Oliveira, A. L. P. R. S.; da Silva, C.; Cardoso, H. P.; Estácio, S.

    2003-08-01

    O projeto Educação em Ciências com Observatórios Virtuais foi concebido pelo Instituto Astronômico e Geofísico da USP, agregando diversas instituições de ensino e pesquisa no país para desenvolver competências diversas na educação fundamental, média e superior utilizando a astronomia como ferramenta multidisciplinar. Este trabalho descreve a participação da MOPPE, escola-piloto do INPE no projeto, no período de 2000-2003. Serão apresentadas 1) a criação de um clube de ciências (1999 a 2001) cujo tema foi a colonização de Marte e 2) a ementa de astronomia trabalhada com as 7a. e 8a. séries do ensino fundamental. A proposta do projeto Colonizando Marte foi estudar diversos aspectos de uma missão interplanetária e construir experiementos que permitissem quantificar esses aspectos. Os resultados obtidos incluiram apresentações nas SBPC Jovem em 2000 e 2001. Discutiremos também as ementas de astronomia trabalhadas desde 2001 e o envolvimento dos alunos com atividades ligadas a astronomia, fora da aula de ciências. A inclusão de astronomia no currículo das últimas séries motivou a participação de mais alunos culminando com a conquista de duas medalhas para alunos da 7a. série na Olimpiada Brasileira de Astronomia em 2002. Houve também um aumento no número de participantes na OBA 2003 e nos projetos de astronomia mais elaborados nas Feira de Ciências de 2001 e 2002. Destacamos em 2003 a inclusão da MOPPE no projeto TIE - Telescopes in Education - da NASA, que utiliza o telescópio do Observatório de Mount Wilson (EUA) para observações remotas em projetos pedagógicos para o ensino de astronomia.

  11. Antarctic meteor observations using the Davis MST and meteor radars

    Science.gov (United States)

    Holdsworth, David A.; Murphy, Damian J.; Reid, Iain M.; Morris, Ray J.

    2008-07-01

    This paper presents the meteor observations obtained using two radars installed at Davis (68.6°S, 78.0°E), Antarctica. The Davis MST radar was installed primarily for observation of polar mesosphere summer echoes, with additional transmit and receive antennas installed to allow all-sky interferometric meteor radar observations. The Davis meteor radar performs dedicated all-sky interferometric meteor radar observations. The annual count rate variation for both radars peaks in mid-summer and minimizes in early Spring. The height distribution shows significant annual variation, with minimum (maximum) peak heights and maximum (minimum) height widths in early Spring (mid-summer). Although the meteor radar count rate and height distribution variations are consistent with a similar frequency meteor radar operating at Andenes (69.3°N), the peak heights show a much larger variation than at Andenes, while the count rate maximum-to-minimum ratios show a much smaller variation. Investigation of the effects of the temporal sampling parameters suggests that these differences are consistent with the different temporal sampling strategies used by the Davis and Andenes meteor radars. The new radiant mapping procedure of [Jones, J., Jones, W., Meteor radiant activity mapping using single-station radar observations, Mon. Not. R. Astron. Soc., 367(3), 1050-1056, doi: 10.1111/j.1365-2966.2006.10025.x, 2006] is investigated. The technique is used to detect the Southern delta-Aquarid meteor shower, and a previously unknown weak shower. Meteoroid speeds obtained using the Fresnel transform are presented. The diurnal, annual, and height variation of meteoroid speeds are presented, with the results found to be consistent with those obtained using specular meteor radars. Meteoroid speed estimates for echoes identified as Southern delta-Aquarid and Sextantid meteor candidates show good agreement with the theoretical pre-atmospheric speeds of these showers (41 km s -1 and 32 km s -1

  12. Estudo da região HII galática NGC 2579

    Science.gov (United States)

    Riffel, R.; Copetti, M. V. F.

    2003-08-01

    Desde a descoberta dos gradientes de abundância química em galáxias espirais, as regiões HII galáticas têm sido intensamente estudadas com o objetivo de determinar a forma do gradiente de abundância química na Via-Láctea. Entretanto, a forma do gradiente galático continua controversa e existem muitas regiões HII que continuam inexploradas. A região HII galática NGC 2579 é um objeto que aparece em imagens Ha, como uma pequena mancha brilhante de aproximadamente 2 segundos de arco de diâmetro a 20 segundos de arco ao leste de RCW 20, sendo NGC 2579 muitas vezes confundida com esta última. Apesar de seu alto brilho superficial, NGC 2579 é um objeto pouco estudado provavelmente por problemas de identificação deste objeto. Como parte de um projeto de reavaliação dos gradientes de abundância química das regiões HII na Via-Láctea, estamos realizando um estudo extensivo das propriedades físicas básicas como temperatura eletrônica, densidade eletrônica e composição química da região HII galática NGC 2579. Analisamos dados espectrofotométricos de fenda longa na faixa de 3700Å a 7750Å obtidos com o telescópio de 1.52 m do ESO, Chile, em 2002. Determinamos a temperatura eletrônica usando a razão entre as linhas do [OIII] (l4959+l5007/l4363) e a densidade eletrônica pela razão entre as linhas do [SII] (l6716/l6731). As abundâncias químicas do O, N, Cl, S, Ne e He foram determinadas. Realizamos um estudo de imagens fotométricas nas bandas UBVRI obtidas em 2000 no observatório astronômico San Pedro Mártir, México, para identificar e classificar as estrelas ionizantes de NGC 2579 e determinar a distância deste objeto.

  13. Espectroscopia de candidatos a remanescentes de aglomerados abertos

    Science.gov (United States)

    Pavani, D. B.; Bica, E.; Ahumada, A. V.; Clariá, J. J.

    2003-08-01

    A pesquisa sobre remanescentes de aglomerados abertos tem despertado grande interesse. Seguindo esta tendência encontramos estudos teóricos e observacionais. Os primeiros baseiam-se em simulações numéricas buscando determinar fração de binárias e distâncias galatocêntricas, tempo de vida e conteúdo estelar. Estes estão relacionados à função inicial de massa e densidade de estrelas, ou seja, se ricos ou pobremente povoados, compactos ou esparsos. No caso observacional procuram-se identificar os remanescentes considerando-se que trazem estas assinaturas de seus percursores. No presente estudo empregamos espectroscopia para analisar oito concentrações pobremente povoadas, previamente classificadas como aglomerados abertos, sendo sete compactas e uma esparsa. As observações foram obtidas através do telescópio de 2,15 m do CASLEO em San Juan, Argentina, em turnos entre 2001 e 2003. Utilizamos uma câmara CCD contendo um chip Tektronics de 1024X1024 pixeis aliado a um espectrógrafo REOSC. O domínio espectral vai de 3700 a 7000 Å. As reduções foram realizadas no Observatório Astronômico de Córdoba (Argentina) usando pacotes IRAF padrões. Determinamos idades, avermelhamentos e tipos espectrais através de comparações com biblioteca de estrelas e de aglomerados. Em alguns casos nossos espectros estavam dominados por estrelas individuais às quais determinamos seus tipos espectrais. Aos oito objetos adicionamos mais cinco da literatura recente analisados via espectro ou diagrama cor-magnitude. O histograma resultante contém idades típicas entre 0.5 e 3 Ganos. Considerando que predominantemente estes objetos encontram-se na vizinhança solar e, portanto, não cruzaram muitas vezes o plano Galático esperamos que a diferença no tempo necessário para dissolução destes prováveis remanescentes seja em função de diferentes massas iniciais.

  14. Poluição atmosférica e atendimentos por pneumonia e gripe em São Paulo, Brasil

    Directory of Open Access Journals (Sweden)

    Martins Lourdes Conceição

    2002-01-01

    Full Text Available OBJETIVO: Investigar os efeitos causados pela poluição atmosférica na morbidade por pneumonia e por gripe em idosos entre 1996 e 1998. MÉTODOS: Foram obtidos dados diários de atendimentos por pneumonia e gripe para idosos em pronto-socorro médico de um hospital-escola de referência no Município de São Paulo, SP, Brasil. Os níveis diários de CO, O3, SO2, NO2 e PM10 foram obtidos na Companhia de Tecnologia de Saneamento Ambiental, e os dados diários de temperatura e umidade relativa do ar foram obtidos no Instituto Astronômico e Geofísico da USP. Para verificar a relação existente entre pneumonia e gripe e poluição atmosférica, utilizou-se o modelo aditivo generalizado de regressão de Poisson, tendo como variável dependente o número diário de atendimentos por pneumonia e gripe e como variáveis independentes as concentrações médias diárias dos poluentes atmosféricos. A análise foi ajustada para sazonalidade de longa duração (número de dias transcorridos, sazonalidade de curta duração (dias da semana, temperatura mínima, umidade média, períodos de rodízio e os atendimentos por doenças não-respiratórias em idosos. RESULTADOS: O3 e SO2 estão diretamente associados à pneumonia e à gripe, independentemente das variáveis de controle. Porém, na análise conjunta, eles perdem sua significância estatística. Pôde-se observar que um aumento interquartil (25%-75% para o O3 (38,80 mig/m³ e SO2 (15,05 mig/m³ levaram a um acréscimo de 8,07% e 14,51%, respectivamente, no número de atendimentos por pneumonia e gripe em idosos. CONCLUSÕES: Os resultados sugerem que a poluição atmosférica promove efeitos adversos para a saúde de idosos.

  15. Modeling of the Enceladus water vapor jets for interpreting UVIS star and solar occultation observations

    Science.gov (United States)

    Portyankina, Ganna; Esposito, Larry W.; Aye, Klaus-Michael; Hansen, Candice J.

    2015-11-01

    ); Porco, C.C. et al. Astron. J. 148, 45 (2014); Spitale, J.N. et al. Nature 521, 57-60 (2015)

  16. Comportamiento del Helio en estrellas químicamente peculiares

    Science.gov (United States)

    Malaroda, S. M.; López García, Z.; Leone, F.; Catalano, F.

    Las estrellas químicamente peculiares (CP) se caracterizan por tener deficiencias y sobreabundancias de algunos elementos químicos de hasta 106 veces la abundancia solar. Además presentan variaciones en las líneas espectrales. Se piensa que ello se debe a que los campos magnéticos presentes en este tipo de estrellas son principalmente dipolares, con un eje de simetría diferente del eje de rotación. La distribución de los elementos sobreabundantes y deficientes no es homogénea sobre la superficie estelar y las variaciones observadas serían una consecuencia directa de la rotación estelar. Entre los elementos con abundancia anómala se encuentra el Helio, cuyas líneas tienen intensidades que no son consistentes con una abundancia normal, que no puede ser determinada del modo usual, o sea, considerando una atmósfera con composición solar. Con el fin de determinar la abundancia de este elemento, se inició un estudio de estrellas anómalas de Helio, Hew y He strong. Además se determinarán las abundancias de otros elementos anómalos como ser el Si, Cr, Mg, Mn y Fe. Las mismas se determinan del modo tradicional, o sea: a) medida de los anchos equivalentes de las líneas de los distintos elementos analizados; b) adopción de la temperatura efectiva, gravedad y abundancia del Helio; c) cálculo del modelo de atmósfera d) comparación con las observaciones y reinicio de un proceso iterativo hasta lograr un acuerdo entre todos los parámetros analizados. Las observaciones se llevaron a cabo en el Complejo Astronómico El Leoncito. Se observaron setenta y ocho estrellas anómalas de Helio. En este momento se está procediendo a calcular las abundancias correspondientes a los distintos elementos químicos. Para ello se hace uso de los modelos de Kurucz, ATLAS9. Los cálculos NLTE de las líneas de Helio se llevan a cabo con el programa MULTI y se compararán con los realizados con el programa WIDTH9 de Kurucz (LTE), con el objeto de resaltar la importancia de

  17. Sistemas Correctores de Campo Para EL Telescopio Cassegrain IAC80

    Science.gov (United States)

    Galan, M. J.; Cobos, F. J.

    1987-05-01

    El proyecto de instrumentación de mayor importancia que ha tenido el Instituto de Astrofisica de Canarias en los últimos afios ha sido el diseflo y construcción del te1escopio IAC8O. Este requería del esfuerzo con junto en mec´nica, óptica y electrónica, lo que facilitó la estructuración y el crecimiento de los respectivos grupos de trabajo, que posteriormente se integraron en departamentos En su origen (1977), el telescopio IAC80 fue concebido como un sistema clásico tipo Cassegrain, con una razón focal F/i 1.3 para el sistema Casse grain y una razón focal F/20 para el sistema Coudé. Posteriormente, aunque se mantuvo la filosofia de que el sistema básico fuera el F/11.3, se consideró conveniente el diseño de secundarios para razones focales F/16 y F/32, y se eliminó el de F/20. Sin embargo, dada la importancia relativa que un foco estrictamente fotográfico tiene en un telescopio moderno, diseñado básicamente para fotometría fotoeléctrica y con un campo util mínimamente de 40 minutos de arco, se decídió Ilevar a cabo el diseño de un secundario F/8 con un sistema corrector de campo, pero que estuviera formado únicamente por lentes con superficies esféricas para que asl su construcción fuera posible en España ó en México. La creciente utilización de detectores bidimensionales para fines de investigación astron6mica y la viabilidad de que en un futuro cercano éstos tengan un área sensible cada vez mayor, hicieron atractiva la idea de tener diseñado un sistema corrector de campo para el foco primario (F/3), con un campo útil mínimo de un grado, y también con la limitante de que sus componentes tuvieron sólamente supérficies esféricas. Ambos diseños de los sis-temas correctores de campo se llevaron a cabo, en gran medida, como parte de un proyecto de colaboración e intercambio en el área de diseño y evaluación de sistemas ópticos.

  18. A Mobile Asteroid Surface Scout (MASCOT) on board the Hayabusa 2 Mission to the near Earth asteroid (162173) Ryugu

    Science.gov (United States)

    Jaumann, R.; Bibring, J. P.; Glassmeier, K. H.; Grott, M.; Ho, T. M.; Ulamec, S.; Schmitz, N.; Auster, H. U.; Biele, J.; Kuninaka, H.; Okada, T.; Yoshikawa, M.; Watanabe, S.; Spohn, T.; Koncz, A.; Hercik, D.; Michaelis, H.; Fujimoto, M.

    2016-12-01

    MASCOT is part of JAXA's Hayabusa 2 asteroid sample return mission that has been launched to asteroid (162173) Ryugu (1,2,3) on Dec 3rd, 2014. It is scheduled to arrive at Ryugu in 2018, and return samples to Earth in 2020. The German Aerospace Center (DLR) developed the lander MASCOT with contributions from CNES (France) (2,3). Ryugu has been classified as a Cg-type (4), believed to be a primitive volatile-rich remnant from the early solar system. Its visible geometric albedo is 0.07±0.01with a diameter of 0.87±0.03 km (5). The thermal inertia indicates thick dust with a cm-sized, gravel-dominated surface layer (5,6). Ryugu shows a retrograde rotation with a period of 7.63±0.01h. Spectral observations indicate iron-bearing phyllosilicates (1) on parts of the surface, suggesting compositional heterogeneity. MASCOT will enable to in-situ map the asteroid's geomorphology, the intimate structure, texture and composition of the regolith (dust, soil and rocks), and its thermal, mechanical, and magnetic properties in order to provide ground truth for the orbiter remote measurements, support the selection of sampling sites, and provide context information for the returned samples (2,3). MASCOT comprises a payload of four scientific instruments: camera, radiometer, magnetometer and hyperspectral microscope (2,3). Characterizing the properties of asteroid regolith in-situ will deliver important ground truth for further understanding telescopic and orbital observations as well as samples of asteroids. MASCOT will descend and land on the asteroid and will change its position by hopping (3). (1) Vilas, F., Astro. J. 1101-1105, 2008; (2) Jaumann, R., et al., SSR, DOI 10.1007/s11214-016-0263-2, 2016; (3) Ho, T.-M. et al., SSR, DOI 10.1007/s11214-016-0251-6, 2016; (4) Bus, S.J., Binzel, R.P. Icarus 158, 2002; (5) Hasegawa, T.G., et al., Astron. Soc. Japan 60, 2008; (6) T.G. Müller, T.G., et al., doi 10.1051/0004-6361/201015599, 2011.

  19. Synchrotron-Based Highest Resolution FTIR Spectroscopy of Azulene, Naphthalene (C_{10}H_8), Indole (C_{8}H_6N) and Biphenyl (C_{12}H_{10})

    Science.gov (United States)

    Albert, S.; Quack, M.; Lerch, Ph.

    2013-06-01

    . Lerch and M. Quack, Faraday Discussions 2011, 150, 71-99. A.G.G.M. Tielens, Annu. Rev. Astron. Astrophys. 2008, 46, 289.

  20. Observational hints of radial migration in disc galaxies from CALIFA

    Science.gov (United States)

    Ruiz-Lara, T.; Pérez, I.; Florido, E.; Sánchez-Blázquez, P.; Méndez-Abreu, J.; Sánchez-Menguiano, L.; Sánchez, S. F.; Lyubenova, M.; Falcón-Barroso, J.; van de Ven, G.; Marino, R. A.; de Lorenzo-Cáceres, A.; Catalán-Torrecilla, C.; Costantin, L.; Bland-Hawthorn, J.; Galbany, L.; García-Benito, R.; Husemann, B.; Kehrig, C.; Márquez, I.; Mast, D.; Walcher, C. J.; Zibetti, S.; Ziegler, B.; Califa Team

    2017-07-01

    , in light of these results we cannot further quantify the importance of radial migration in shaping spiral galaxies, and other processes, such as recent star formation or satellite accretion, might play a role. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).Table 1 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/604/A4

  1. VizieR Online Data Catalog: PMA Catalogue (Akhmetov+, 2017)

    Science.gov (United States)

    Akhmetov, V. S.; Fedorov, P. N.; Velichko, A. B.; Shulga, V. M.

    2017-06-01

    calculated above. In case of any problems or questions, please contact by e-mail V.S. Akhmetov (akhmetovvs(at)gmail.com or akhmetov(at)astron.kharkov.ua). (1 data file).

  2. Annual Variations of the Geomagnetic Field in the Earth's Polar Regions

    Science.gov (United States)

    Ou, Jiaming; Du, Aimin

    2017-04-01

    -known fundamental north-south and seasonal anti-correlations is discussed. Reference 1. Malin, S. R. C., A. Mete Isikaka (1976), Annual variation of the geomagnetic field, J. R. Astron. Soc., 47, 445-457, doi: 10.1111/j.1365-246X.1976.tb07096.x. 2. Stauning, P. (2011), Determination of the quiet daily geomagnetic variations for polar regions, J. Atmos. Sol-Terr. Phy., 73, 2314-2330, doi:10.1016/j.jastp.2011.07.004.

  3. A proof of the cancellation of the redistribution tidal potential effects on the rotation of an elastic Earth model

    Science.gov (United States)

    Baenas, Tomás; Escapa, Alberto; Ferrándiz, Jose Manuel

    2014-05-01

    2010-22039-C02-02, and Universidad de Alicante project GRE11-08. Escapa, A., Getino, J., & Ferrándiz, J. M. 2004, Proc. Journées Sys. Ref., Ed. N. Capitaine, Paris, 70 Ferrándiz, J. M., Baenas, T., & Escapa, A. 2012, Geophys. Res. Abs., 14, EGU2012-6175 Krasinsky, G. A. 1999, Celest. Mech. Dyn. Astron., 75, 39 Lambert, S. & Mathews, P. M. 2006, A&A, 453, 363

  4. Relativistic and correlation effects in electron impact excitation of forbidden transitions of OII

    Energy Technology Data Exchange (ETDEWEB)

    Montenegro, Maximiliano [Department of Astronomy, Ohio State University, Columbus, OH 43210 (United States); Department of Education, Ohio State University, Columbus, OH 43210 (United States); Eissner, Werner [Institut fuer Theoretische Physik, Teilinstitut 1, 70550 Stuttgart (Germany); Nahar, Sultana N [Department of Astronomy, Ohio State University, Columbus, OH 43210 (United States); Pradhan, Anil K [Department of Astronomy, Ohio State University, Columbus, OH 43210 (United States)

    2006-04-28

    We investigate relativistic and correlation effects in electron impact excitation of singly ionized oxygen using the Breit-Pauli R-matrix method. The intermediate coupling close-coupling calculations are carried out using a 16-level target representation dominated by the electronic configurations 1s{sup 2}2s{sup 2}2p{sup 3}, 1s{sup 2}2s2p{sup 4}, 1s{sup 2}2s{sup 2}2p{sup 2}3s. Resonance structures are delineated in detail to ascertain the effect on averaged collision strengths. Convergence of the partial wave summation is ensured for non-dipole transitions in the R-matrix calculations. The present results differ significantly from the similar Breit-Pauli R-matrix calculations by McLaughlin and Bell (1998 J. Phys. B: At. Mol. Opt. Phys. 31 4317-29), but are essentially in agreement with the LS coupling results of Pradhan (1976a J. Phys. B: At. Mol. Opt. Phys. 9 433-43, 1976b Mon. Not. R. Astron. Soc. 177 31-8). A comprehensive study of the detailed energy behaviour of all forbidden transitions among the five levels of the ground configuration, i.e. 2s2p{sup 3}({sup 4}S{sup o}{sub 3/2}, {sup 2}D{sup o}{sub 5/2,3/2}, {sup 2}P{sup o}{sub 3/2,1/2}) shows that the finestructure collision strengths do not significantly depart from the values obtained from a purely LS {yields} LSJ transformation, and relativistic effects are therefore small. We find that the Maxwellian-averaged effective collision strengths for the ten transitions also differ from the previous work, most likely due to more extensive delineation of resonances in the present work. However, the differences are largely systematic and therefore the OII line intensity ratios are not significantly affected. We also obtain an excellent agreement between the present-calculated cross sections for the {sup 4}S{sup o} - {sup 2}D{sup o} transition and the experimental merged beam measurements.

  5. Simulação de ejeções de massa coronal

    Science.gov (United States)

    Corsini, M. A.; Silva, A. V. R.

    2003-08-01

    Ejeções de massa coronal (EMC) são bolhas gigantes de gás permeadas por campos magnéticos que são ejetadas do Sol durante um período de várias horas. Caso estas ejeções atinjam a Terra, geralmente, causam uma série de distúrbios às comunicações de longa distância e navegação, além de danos a satélites e transformadores. Portanto, é desejável que sejamos capazes de prever quando estas ejeções atingirão a Terra. Para tanto, é necessário um bom entendimento dos mecanismos causadores das ejeções e, principalmente, de como se dá a propagação das EMC e sua interação com o vento solar que permeia o meio interplanetário. Nesse sentido foi desenvolvido um programa computacional para resolver as equações MHD (Magneto-Hidro-Dinâmica) que regem a evolução das EMC. Primeiramente foram estabelecidas as condições necessárias para descrever o vento solar, no estado estacionário, que permeia todo o meio interplanetário. Num primeiro momento, resolveu-se o sistema de equações para o caso do vento isotérmico, conhecida como a solução de Parker, a fim de testarmos o modelo. Então, foi considerado o caso do vento solar com temperatura variável no meio interplanetário. Este resultado foi utilizado como a base de nosso sistema em seu instante inicial. Posteriormente foram feitas as considerações necessárias para descrever a propagação da Ejeção de Massa Coronal. As EMC foram simuladas como um aumento de densidade e temperatura local na coroa solar. A órbita e a posição da Terra foram incluídas no sistema. Os dados gerados possibilitaram uma análise da evolução da EMC pelo meio interplanetário até encontrar-se com a Terra. Os perfis de densidade e temperatura a 1 Unidade Astronômica são comparados com os dados de satélites reportados na literatura.

  6. Models of dark matter halos based on statistical mechanics: The fermionic King model

    Science.gov (United States)

    Chavanis, Pierre-Henri; Lemou, Mohammed; Méhats, Florian

    2015-12-01

    We discuss the nature of phase transitions in the fermionic King model which describes tidally truncated quantum self-gravitating systems. This distribution function takes into account the escape of high-energy particles and has a finite mass. On the other hand, the Pauli exclusion principle puts an upper bound on the phase-space density of the system and stabilizes it against gravitational collapse. As a result, there exists a statistical equilibrium state for all accessible values of energy and temperature. We plot the caloric curves and investigate the nature of phase transitions as a function of the degeneracy parameter in both microcanonical and canonical ensembles, extending the work of Chavanis [Int. J. Mod. Phys. B 20, 3113 (2006)] for box-confined configurations. We consider stable and metastable states and emphasize the importance of the latter for systems with long-range interactions. Phase transitions can take place between a "gaseous" phase unaffected by quantum mechanics and a "condensed" phase dominated by quantum mechanics. The phase diagram exhibits two critical points, one in each ensemble, beyond which the phase transitions disappear. There also exists a region of negative specific heats and a situation of ensemble inequivalence for sufficiently large systems. In the microcanonical ensemble, gravitational collapse (gravothermal catastrophe) results in the formation of a small degenerate object containing a small mass. This is accompanied by the expulsion of a hot envelope containing a large mass. In the canonical ensemble, gravitational collapse (isothermal collapse) leads to a small degenerate object containing almost all the mass. It is surrounded by a tenuous envelope. We apply the fermionic King model to the case of dark matter halos made of massive neutrinos following the work of de Vega, Salucci, and Sanchez [Mon. Not. R. Astron. Soc. 442, 2717 (2014)]. The gaseous phase describes large halos and the condensed phase describes dwarf halos

  7. Conhecimento Científico e Cotidiano em Astronomia: Uma Investigação com Alunos da Educação Básica

    Science.gov (United States)

    Vieira, J. B.; Longhini, M. D.

    2011-12-01

    Este texto apresenta resultados de uma investigação que teve como objetivo, investigar como os conhecimentos científicos e do cotidiano relacionados a essa área de conhecimento apresentam na escola de Educação Básica, especialmente, em alunos do Ensino Médio prestes a deixar Educação Básica. Para realização da pesquisa, utilizamos como recurso metodológico a aplicação de um questionário estruturado contendo 47 questões, organizadas em duas categorias: Conhecimento Cotidiano e Conhecimento Científico. As questões da categoria “Conhecimento Cotidiano” possuíam afirmações relacionadas a crendices, contos populares, especulações e temáticas do gênero, as quais, geralmente, estão fora do círculo de discussão da comunidade científica, talvez por não serem consideradas como objeto de estudo da ciência. As questões da categoria “Conhecimento Científico” são relacionadas a conteúdos específicos de Astronomia, as quais são compartilhadas pela comunidade científica e aceitas, pelo menos provisoriamente, como possuindo fundamentação científica. Concluímos que, possuem ainda concepções de temas Astronômicos persistentes à mudança, por exemplo, fases da Lua relacionadas à melhor período para corte de cabelo e também para plantio; estrela cadente e ocasião perfeita para se fazer um pedido. Entretanto, podemos observar no que diz respeito a mitos e superstições, que quase não existe influência destes entre os alunos. Portanto, ao trabalharmos com os alunos determinados conceitos científicos, é importante lembrarmos que o professor não opera no vazio; os alunos são sujeitos de saberes, práticas e, dessa forma constroem e reconstroem saberes. Cabe ao professor ouvir os estudantes reconstruindo junto deles conceitos científicos. Acreditamos que o ensino de Ciências na Educação Básica deve lidar criticamente com o conhecimento cotidiano e científico e, assim, efetivar a Ciência como disciplina educativa

  8. Escribir contra la ciudad: fotos y texto en Prosa del observatorio de Julio Cortázar

    Directory of Open Access Journals (Sweden)

    Marcy Schwartz

    2012-10-01

    Full Text Available De los muchos proyectos fotográficos de Julio Cortázar, Prosa del observatorio es el único en que él es el autor de las fotos tanto como del ensayo. Una de las obras menos estudiadas de Cortázar, Prosa presenta fotos de los observatorios astronómicos en Jaipur y Delhi diseñados por Jai Singh en el siglo XVIII. Este artículo explora la dinámica verbal-visual de Prosa en el contexto de la mirada urbana que pesa sobre ambos discursos (lo verbal y lo visual. La perspectiva occidental parisina se enfrenta con la perspectiva oriental de Jaipur para desmantelar el imperativo urbano.Parmi les multiples projets photographiques menés pas Julio Cortázar, Prose de l’Observatoire est le seul où il est à la fois auteur des photographies et de l’essai. L’une des œuvres le moins étudiées par Cortázar, Prose présente des photographies des observatoires astronomiques de Jaipur et de Delhi, dessinés par Jai Singh au XVIIIe siècle. Cet article explore la dynamique visuel/verbal de Prose, dans le conteste d’un regard urbain qui pèse sur les deux discours (le verbal et le visuel. La perspective orientale parisienne se voit confrontée à la perspective orientale de Jaipur, pour démanteler ainsi l’impératif urbain.Of Julio Cortázar’s many photographic projects, only in Prosa del observatorio is he both author and photographer. One of the least studied works by Cortázar, Prosa presents photos of the astronomical observatories in Jaipur and Delhi designed by Jai Singh in the eighteenth century. This article explores the verbal-visual dynamic in Prosa in the context of the urban gaze that weighs on both the verbal and the visual discourse. The Western, Parisian perspective comes up against the Asian perspective of Jaipur to undermine the urban imperative.

  9. Developing the Planetary Science Virtual Observatory

    Science.gov (United States)

    Erard, Stéphane; Cecconi, Baptiste; Le Sidaner, Pierre; Henry, Florence; Chauvin, Cyril; Berthier, Jérôme; André, Nicolas; Génot, Vincent; Schmitt, Bernard; Capria, Teresa; Chanteur, Gérard

    2015-08-01

    In the frame of the Europlanet-RI program, a prototype Virtual Observatory dedicated to Planetary Science has been set up. Most of the activity was dedicated to the definition of standards to handle data in this field. The aim was to facilitate searches in big archives as well as sparse databases, to make on-line data access and visualization possible, and to allow small data providers to make their data available in an interoperable environment with minimum effort. This system makes intensive use of studies and developments led in Astronomy (IVOA), Solar Science (HELIO), and space archive services (IPDA).The current architecture connects existing data services with IVOA or IPDA protocols whenever relevant. However, a more general standard has been devised to handle the specific complexity of Planetary Science, e.g. in terms of measurement types and coordinate frames. This protocol, named EPN-TAP, is based on TAP and includes precise requirements to describe the contents of a data service (Erard et al Astron & Comp 2014). A light framework (DaCHS/GAVO) and a procedure have been identified to install small data services, and several hands-on sessions have been organized already. The data services are declared in standard IVOA registries. Support to new data services in Europe will be provided during the proposed Europlanet H2020 program, with a focus on planetary mission support (Rosetta, Cassini…).A specific client (VESPA) has been developed at VO-Paris (http://vespa.obspm.fr). It is able to use all the mandatory parameters in EPN-TAP, plus extra parameters from individual services. A resolver for target names is also available. Selected data can be sent to VO visualization tools such as TOPCAT or Aladin though the SAMP protocol.Future steps will include the development of a connection between the VO world and GIS tools, and integration of heliophysics, planetary plasma and reference spectroscopic data.The EuroPlaNet-RI project was funded by the European

  10. Tidal Synchronization of Close-in Satellites and Exoplanets, Host Stars and Mercury

    Science.gov (United States)

    Ferraz-Mello, Sylvio

    2014-05-01

    This paper deals with an application of the creep tide theory (Ferraz-Mello, Cel. Mech. Dyn. Astron. 116, 109, 2013) to the rotation of close-in satellites, Mercury, close-in exoplanets and their host stars. The solutions show different behaviors in the two extreme cases: low-viscosity close-in gaseous planets and stars (high relaxation factor) and high-viscosity rocky satellites and planets (low relaxation factor). The rotation of close-in gaseous planets follows the classical Darwinian pattern: it is tidally driven towards a synchronous solution when the orbit is circular, but to a super-synchronous solution, with frequency (1+6e^2) times the orbital mean-motion, when the orbit is elliptic. The rotation of rocky bodies, however, may be driven to several attractors whose frequencies are 1/2, 1, 3/2, 2, 5/2,… times the mean-motion. The number of attractors increases with the viscosity of the body and the orbital eccentricity. The final stationary state depends on the initial conditions and on the eccentricity of the orbits. The well-known case of Mercury, whose rotational period is 2/3 of the orbital period (3/2 attractor), is a consequence of the nonzero orbital eccentricity and of the relaxation factor of the planet (large enough to avoid the 2/1 attractor, but small enough to be trapped in the 3/2 one). Mercury's relaxation factor can thus be estimated to lie in the interval 4.6-27 nHz (which allows Q to be roughly constrained to the interval 5

  11. The Resolved Asteroid Program - Size, shape, and pole of (52) Europa

    Science.gov (United States)

    Merline, W. J.; Drummond, J. D.; Carry, B.; Conrad, A.; Tamblyn, P. M.; Dumas, C.; Kaasalainen, M.; Erikson, A.; Mottola, S.; Ďurech, J.; Rousseau, G.; Behrend, R.; Casalnuovo, G. B.; Chinaglia, B.; Christou, J. C.; Chapman, C. R.; Neyman, C.

    2013-07-01

    With the adaptive optics (AO) system on the 10 m Keck-II telescope, we acquired a high quality set of 84 images at 14 epochs of asteroid (52) Europa on 2005 January 20, when it was near opposition. The epochs covered its 5.63 h rotation period and, by following its changing shape and orientation on the plane of sky, we obtained its triaxial ellipsoid dimensions and spin pole location. An independent determination from images at three epochs obtained in 2007 is in good agreement with these results. By combining these two data sets, along with a single epoch data set obtained in 2003, we have derived a global fit for (52) Europa of diameters a × b × c = (379 × 330 × 249) ± (16 × 8 × 10) km, yielding a volume-equivalent spherical-diameter of √abc3 =315±7km, and a prograde rotational pole within 7° of [RA; Dec] = [257°; +12°] in an Equatorial J2000 reference frame (Ecliptic: 255°; +35°). Using the average of all mass determinations available for (52) Europa, we derive a density of 1.5 ± 0.4 g cm-3, typical of C-type asteroids. Comparing our images with the shape model of Michalowski et al. (2004, Astron. Astrophys. 416, 353), derived from optical lightcurves, illustrates excellent agreement, although several edge features visible in the images are not rendered by the model. We therefore derived a complete 3-D description of (52) Europa's shape using the KOALA algorithm by combining our 18 AO imaging epochs with 4 stellar occultations and 49 lightcurves. We use this 3-D shape model to assess these departures from ellipsoidal shape. Flat facets (possible giant craters) appear to be less distinct on (52) Europa than on other C-types that have been imaged in detail, (253) Mathilde and (511) Davida. We show that fewer giant craters, or smaller largest-sized craters, is consistent with its expected impact history. Overall, asteroid (52) Europa is still well modeled as a smooth triaxial ellipsoid with dimensions constrained by observations obtained over

  12. Coordination of NEO Observers in South-America

    Science.gov (United States)

    Tancredi, G.

    At present the discovery of NEOs is concentrated in the Northern Hemisphere. None of the 6 existing survey programs can reach declinations below -30deg. Nevertheless, there are two small surveys ready to start in the near future in the southern hemisphere: an extension of the Catalina Sky Survey using the Uppsala Schmidt in Siding Spring and the Project BUSCA in Uruguay. Many of the NEOs discovered by the northern surveys could reach the southern sky, with declinations unreachable for a northern observer. Furthermore, the recovery of an asteroid in subsequent oppositions could come indistinctly in the northern and southern sky. A network of well-equipped observers in the southern region is then a must in a campaign to catalog the NEO population. In view of this situation, the Planetary Society, through its NEO grant, have already supported many observers in the Southern Hemisphere. The planetary science community in South America has considerably grown in the last 10 years. We have well-known research groups in Argentina, Brazil and Uruguay. Those groups have established many scientific links by exchanging graduate students and through several meetings. In particular, we have already hold two Workshop in Planetary Science in South America in 1999 (La Plata, Argentina) and 2000 (Montevideo, Uruguay) with more than 25 participants each. Recently, in February 2002, we organized a Workshop of NEO observers in Montevideo with the participation of more than 20 professional and amateurs observers from: Argentina: Obs. Ast. Felix Aguilar - Yale University (San Juan) and CRICYT (Mendoza); Brazil: Obs. Abraes de Moraes (San Pablo), Obs. Wykrota (Belo Horizonte) and Observatorio Nacional (Rio de Janeiro); Paraguay: Obs. Nacional de Asuncion and Sociedad de Estudios Astronómicos (Asunción) Uruguay: Depto. Astronomía - Fac. Ciencias, Obs. Ast. Los Molinos and Obs. Kappa Crucis (Montevideo). Among the resolutions of the Workshop, we highlight: * Creation of the "Asociaci

  13. Evaluación de la escala Borg de esfuerzo percibido aplicada a la rehabilitación cardiaca Instrument evaluation of Borg's perceived exertion scale in cardiac rehabilitation

    Directory of Open Access Journals (Sweden)

    Natalie Burkhalter

    1996-12-01

    Full Text Available La escala Borg de esfuerzo percibido mide la gama entera del esfuerzo que el individuo percibe al hacer ejercicio. Esta escala da criterios para hacerle ajustes a la intensidad de ejercicio, o sea, a la carga de trabajo, y así pronosticar y dictaminar las diferentes intensidades del ejercicio en los deportes y en la rehabilitación médica (BORG, 1982. También se puede usar tanto en el atletismo, en la astronáutica, la industria y ambientes militares, como en las situaciones cotidianas. El concepto del esfuerzo percibido es una valoración subjetiva que indica la opinión del sujeto respecto a la intensidad del trabajo realizado (MORGAN, 1973. El sujeto que hace el ejercicio debe asignar un número del 1 al 20, para representar la sensación subjetiva de la cantidad de trabajo desempeñado. La escala es una herramienta valiosa dentro del ámbito del desempeño humano, en que a menudo la consideración importante no es tanto "lo que haga el individuo" "sino" "lo que cree que hace" (MORGAN, 1973.Borg's perceived exertion scale measures the extent of perceived exertion which a person experiences during exercise. The perceived exertion scale is used to adjust exercise intensity (workload for predictions and prescriptions of exercise intensities in sports and medical rehabilitation (BORG, 1982. In addition, Borg's scale can be used in the athletic arena, space, industry, military settings, or under everyday circumstances. The concept of perceived exertion is a subjective rating, indicating the subject's opinion about the intensity of the work being performed (MORGAN, 1973. The task of exercising subjects is to assign a number (from 1-20 to represent the subjective sensation of the amount of work being performed. This is a valuable tool in human performance setting, where an important consideration is not "what the individual is doing, but what he thinks and is doing" (MORGAN, 1973.

  14. A post-Rosetta understanding of polarimetric observations of comets

    Science.gov (United States)

    Levasseur-Regourd, A. Chantal; Ciarletti, Valérie; Hadamcik, Edith; Lasue, Jérémie; Mannel, Thurid

    2017-04-01

    -Regourd, 2003, Icarus 166, 188-194. [4] Ciarletti et al., 2015, Astron. Astrophys. 583, A40. [5] Lasue et al., 2009, Icarus 199, 129-144. [6] Mannel et al., 2016, MNRAS 462, S 304-S311.

  15. On the secular recession of the Earth-Moon system as an azimuthal gravitational phenomenon

    Science.gov (United States)

    Nyambuya, G. G.; Makwanya, T.; Tuturu, B. A.; Tsoka, W.

    2015-07-01

    We here apply the ASTG-model to the observed secular trend in the mean Sun-(Earth-Moon) and Earth-Moon distances thereby providing an alternative explanation as to what the cause of this secular trend may be. Within the margins of observational error; for the semi-major axis rate of the Earth-Moon system, in agreement with observations (of Standish and Kurtz, Proceedings IAU Colloquium, IAU, pp. 163-179, Cambridge University Press, Cambridge, 2005), we obtain a value of about +(5.10±0.10) cm/yr. The ASTG-model predicts orbital drift as being a result of the orbital inclination and the Solar mass loss rate. The Newtonian gravitational constant G is assumed to be an absolute time constant. Krasinsky and Brumberg (Celest. Mech. Dyn. Astron. 90(3-4):267-288, 2004); Standish and Kurtz (2005) reported for the Earth-Moon system, an orbital recession from the Sun of about +(15.00±4.00) cm/yr and +(7.00±2.00) cm/yr respectively; while Williams et al. (Phys. Rev. Lett. 93:261101, 2004); Williams and Boggs (Proceedings of 16th International Workshop on Laser Ranging, Space Research Centre, Polish Academy of Sciences, Poland, 2009), Williams et al. (Planet. Sci. 3(1):2, 2014) report for the Moon, a semi-major axis rate of about +(38.08±0.04) mm/yr from the Earth. The predictions of the ASTG-model for the Earth-Moon system agrees very well with those the findings of Standish and Kurtz (2005), Krasinsky and Brumberg (2004). The lost orbital angular momentum for the Earth-Moon system—which we here hypothesize to be gained as spin by the two body Earth-Moon system; this lost angular momentum accounts very well for the observed Lunar drift, therefore, one can safely say that the ASTG-model does to a reasonable degree of accuracy predict the observed Lunar semi-major axis rate of about +(38.08±0.04) mm/yr from the Earth.

  16. Questões mais freqüentes na área de astronomia

    Science.gov (United States)

    Segundo, H. A. S.; Garcia, G. C.; Caretta, C. A.; Lima, F. P.

    2003-08-01

    É amplamente reconhecido que as pessoas em geral têm grande fascínio e interesse pela Astronomia. Por outro lado, o conteúdo dessa área incluído no ensino formal está longe de ser abrangente e suficiente para suprir a demanda. Esse interesse permite otimizar a divulgação e o ensino não formal de Astronomia aliando a adequação do conteúdo à expectativa das pessoas. Nesse intuito, nosso trabalho busca mapear que assuntos da Astronomia despertam mais a atenção e o interesse das pessoas e o quanto disso é estimulado pela mídia, que freqüentemente aproveita-se desse interesse de forma sensacionalista, trazendo contribuições positivas e negativas. Para esta avaliação, utilizamos as pesquisas específicas e de caracterização do público que freqüentou o MAst nos anos de 2001 a 2003, pesquisa das matérias de Astronomia veiculadas na mídia escrita da cidade do Rio de Janeiro no mesmo período, além da base de dados do programa Pergunte a um astrônomo, realizado no Observatório Nacional nos anos de 1997 a 1999. Para a análise dos dados, dividimos as perguntas em dez categorias, cada uma com suas subcategorias, tomando como referência as divisões, comissões e grupos de trabalho da IAU. Apresentamos neste trabalho os resultados dessa pesquisa, que incluem, entre outros, a predominância de questões nas categorias Observação do Céu e Sistemas Planetários enquanto nos jornais dominam as notícias de Sistemas Planetários e Espaço & Astronáutica. Outro resultado interessante indicou que as dúvidas de crianças do ensino fundamental se concentram em algumas categorias enquanto as questões de adultos são mais distribuídas por todas as categorias. Os resultados dessa pesquisa serão aplicados diretamente no aperfeiçoamento das atividades do Programa de Observação de Céu, bem como na elaboração de novos projetos e eventos realizados no MAst.

  17. Particle Sizes and Self Gravity Wakes in Saturn's A Ring

    Science.gov (United States)

    Jerousek, R. G.; Colwell, J. E.; Esposito, L. W.; Nicholson, P. D.

    2015-12-01

    The Cassini Ultraviolet Imaging Spectrograph (UVIS) and Visual and Infrared Mapping Spectrometer (VIMS) have measured normal optical depths throughout Saturn's rings by stellar occultations covering a wide range of viewing geometries. The UVIS photometer has an effective wavelength of 0.15 µm and a relatively wide (6.0 mrad × 6.4 mrad) field-of-view. VIMS, in occultation mode, measures at an effective wavelength of 2.9 µm and over a single pixel of angular dimensions 0.25 mrad × 0.5 mrad. Occultations measured by VIMS at the same viewing geometry as UVIS occultations overstate the optical depth if particles smaller than 1.22λVIMS/2θ ~ 8.36 mm are present because light diffracted out of the VIMS pixel by those particles is not replaced by neighboring particles. By measuring differential optical depths one can probe the parameters of the ring particle size distribution (i.e. Zebker et al. 1985, Icarus, 64, 531-548). The technique is complicated, however, by the geometric dependence of the optical depth imposed by the non-axisymmetric self-gravity wakes, which are ephemeral elongated aggregates, deformed by Keplerian shear. Beginning with the granola bar wake model of Colwell et al. (2006, Geophys. Res. Lett., 33, L07201), we introduce a free parameter τsmall which represents the excess normal optical depth measured by VIMS due to sub-cm particles between the opaque wakes and combine VIMS and UVIS occultations for particle size analysis while simultaneously determining the properties of the wakes. We find that throughout the A Ring the wake properties generally agree with previously published results (Colwell et al. 2006, Hedman et al. 2007, Astron. J., 133, 2624-2629). We find a significant fraction of sub-cm particles in the inner and outer A Ring and in the troughs of density waves near strong Lindblad resonances. While wake properties vary in the halo regions surrounding these resonances, the abundance of sub-cm particles varies little from 124

  18. Identification of Postclassic Maya Constellations from the Venus Pages of the Dresden Codex

    Directory of Open Access Journals (Sweden)

    Changbom Park

    2010-01-01

    Full Text Available Ancient Mayan civilization, flourished from 1200 B.C. to 1500 A.D., has left numerous hieroglyphic texts on astronomical observations and calendar. In particular, the Dresden Codex contains the most details of such ancient Mayan heritage. Page 24 and those from 46 to 50 of the Dresden Codex describe the Mayan Venus calendar along with the augural descriptions. We note that the calendar in Dresden Codex is Venus-solar calendar. Our work focuses on the possibility that the calendar was made to work in conjunction with the periodic appearance of constellations on the sky. By analyzing the descriptions in the Venus pages, we propose that the columns in each page describe the motion of Venus with respect to major constellations at dates corresponding to special events while the calendar dates increase horizontally in the synodic period of Venus. We present twenty Mayan constellations identified from the Venus pages assuming that the first date of page 46 is February 6, 1228. We also report our understanding of verb expressions about the relative movement of constellations and Venus.La civilización maya, que floreció del 1200 a.C. a 1500 d.C., dejó numerosos textos jeroglíficos sobre el calendario y observaciones astronómicos. El Códice de Dresde, en particular, contiene el más detallado de dichos antiguos legados mayas. Las páginas 24 y 46 a 50 de dicho códice describen el calendario de Venus con los augurios correspondientes. Nosotros hemos notado que éste es un calendario Venus-Solar, y nuestro trabajo se enfoca sobre la posibilidad de que estuviera hecho para trabajar en conjunción con la aparición de determinadas constelaciones en el cielo. Es a través del análisis y descripción de las páginas de Venus que proponemos que las columnas en cada página describen el movimiento de Venus respecto de constelaciones mayores, en fechas que corresponden a eventos especiales, mientras que las fechas calendáricas se incrementan

  19. Usina de ciências: um espaço pedagógico para aprendizagens múltiplas

    Science.gov (United States)

    Martin, V. A. F.; Poppe, P. C. R.; Orrico, A. C. P.; Pereira, M. G.

    2003-08-01

    Entendemos que o Ensino de Astronomia é especialmente apropriado para motivar os alunos e aprofundar conteúdos em diversas áreas do conhecimento, pois envolve temas ligados à Física, Matemática, Química, Computação, Tratamento de Imagens e Instrumentação de Alta Precisão, além daqueles pertinentes as áreas de Geografia, História e Antropologia. Contudo, apesar do caráter interdisciplinar que esta ciência possui, a realidade atual é que a maioria dos professores em sala de aula não foram devidamente capacitados, durante o período de formação acadêmica, para ministrar conteúdos de Astronomia nos atuais Ensinos Fundamental e Médio. Neste trabalho, discutiremos de maneira ampla, num primeiro momento, a realidade do atual ensino de ciências praticado no Estado da Bahia, apontando por dependência administrativa, o crescimento e a redução do número de escolas, da taxa de analfabetismo por faixa etária, da escolarização, do atendimento, da aprovação, reprovação e abandono, de equipamentos e laboratórios e o grau de formação dos nossos atuais professores em pleno exercício de atividade docente. Num segundo momento, discutiremos o papel do Observatório Astronômico Antares/UEFS dentro desse contexto, ou seja, suas ações implementadas ao longo dos últimos anos e em particular, o recente projeto de extensão Ensino e Difusão de Astronomia, financiado pela Fundação Vitae, que procura traduzir no lúdico, no brincar de ciências, um espaço pedagógico para aprendizagens múltiplas. Neste, o papel do professor multiplicador associado ao laboratório de kits didáticos, de fácil construção e manipulação (alguns dos quais serão mostrados), perfazem os principais veículos para o desenvolvimento de conhecimentos, atitudes, habilidades e valores que preparam os nossos alunos para a carreira técnico-científica e para sua participação crítica e criativa na Sociedade.

  20. Astronomia cultural e meio ambiente segundo uma abordagem holística

    Science.gov (United States)

    Jafelice, L. C.

    2003-08-01

    Neste trabalho ampliamos a discussão da abordagem holística para o ensino de astronomia que temos desenvolvido nos últimos anos, analisamos novos resultados e apresentamos exemplos práticos para interessados em experimentá-la. A constatação básica a orientar este enfoque é que cursos introdutórios em astronomia costumam ser excessiva e prematuramente técnicos, além de assumirem uma visão tradicional, muito estreita, do que seja educação científica, herdada da era cartesiana e positivista da ciência. Fundamentamos porque é importante que elementos de astronomia cultural ofereçam o mote e constituam o eixo norteador daqueles cursos e porque é urgente revermos a visão que temos da relação entre astronomia e meio ambiente. Um ponto central nesta abordagem é explorar formas de reativar e atualizar uma relação orgânica com o meio e excitar a consciência de nossa inevitável e profunda interdependência com ele em nível cósmico. Neste trabalho exemplificamos a possibilidade de concretização desta proposta em três diferentes situações: disciplinas de cursos de licenciatura em geografia e em física; escolas de nível fundamental; e, neste caso ainda a ser implementada, comunidades carentes. Estes casos envolvem públicos e espaços diferenciados para educação formal e não-formal. Dos casos já implementados, destacamos os resultados alcançados pelos alunos: enriquecimento cultural, aprendizagem significativa de conteúdos astronômicos tradicionais; mudanças de comportamento, incorporando contato diário com o céu; e freqüentes vivências de sentimentos empáticos que redirecionam a relação com a natureza e a consciência ecológica global. Além disto, para interessados em aplicar esta proposta, também socializamos procedimentos e cuidados para a implementação de ações alternativas consonantes com a mesma. (PPGECNM/UFRN; PRONEX/FINEP; NUPA/USP; Temáticos/FAPESP)

  1. Variaciones seculares de período en las RR Lyrae de ω~Centauri

    Science.gov (United States)

    Marraco, H. G.; Milesi, G. E.

    Utilizando 689 observaciones de 35 estrellas RR Lyrae del cúmulo globular ω Centauri hemos obtenido nuevas determinaciones de sus períodos y sus correspondientes variaciones seculares. Las observaciones fueron obtenidas de la literatura con la excepción de un grupo 66 determinaciones que se presentan por vez primera aquí. Utilizando el parámetro testigo σ descripto en Marraco & Muzzio (Publ. Astron. Soc. Pacific 92, 700, 1980), hemos realizado un ajuste bidimensional en P y β (donde β es la variación secular del período). Con este fin la totalidad de las 689 observaciones fueron llevadas a un sistema fotométrico común. Para esto se realizó un cuidadoso análisis de los numerosos errores en la identificación de las estrellas de las series de comparación. Los resultados de los ajustes bidimensionales fueron analizados utilizando técnicas de procesamiento de imágenes. Con este fin el parámetro de ajuste σ fue representado como función de P y β. En las imágenes resultantes se buscaron los mínimos y al menor de ellos se lo aceptó como período instantáneo verdadero y su variación secular β. La determinación precisa de cada parámetro se realizó mediante ajuste de gaussianas y se determinaron sus errores. A modo de ejemplo la variable #8 fue analizada en una matriz de 501 × 501 elementos representando el parámetro σ para valores comprendidos entre 0,521034 < P < 0,521534 dias y -150×10-10 < β < +150×10-10 dias/dia. El mejor período instantáneo (correspondiente a la época DJ=2.426.908) y su variación secular son P = 0,5212859±0,0000001 días y β 14,012±,010×10-10 días/día respectivamente. Con estos valores el parámetro testigo resulta σ= 0,127 . Si no se tiene en cuenta la variación secular del período y se busca aquél de mejor ajuste para β = 0, se obtiene P = 0,5212960 días, pero entonces el parámetro de ajuste resulta tan alto como σ = 0,23 .

  2. MATISSE: alignment, integration, and test phase first results

    Science.gov (United States)

    Allouche, F.; Robbe-Dubois, S.; Lagarde, S.; Cruzalèbes, P.; Antonelli, P.; Bresson, Y.; Fantei-Caujolle, Y.; Marcotto, A.; Morel, S.; Beckmann, U.; Bettonvil, F.; Berio, Ph.; Heininger, M.; Lehmitz, M.; Agocs, T.; Brast, R.; Elswijk, E.; Ives, D.; Meixner, K.; Laun, W.; Mellein, M.; Neumann, U.; Bailet, C.; Clausse, J.-M.; Matter, A.; Meilland, A.; Millour, F.; Petrov, R. G.; Accardo, M.; Bristow, P.; Frahm, R.; Glindemann, A.; Gonzáles Herrera, J.-C.; Lizon, J.-L.; Schöller, M.; Graser, U.; Jaffe, W.; Lopez, B.

    2016-08-01

    MATISSE (Multi AperTure mid-Infrared SpectroScopic Experiment) is the spectro-interferometer for the VLTI of the European Southern Observatory, operating in near and mid-infrared, and combining up to four beams from the unit or the auxiliary telescopes. MATISSE will offer new breakthroughs in the study of circumstellar environments by allowing the multispectral mapping of the material distribution, the gas and essentially the dust. The instrument consists in a warm optical system (WOP) accepting four optical beams and relaying them after a dichroic splitting (for the L and M- and N- spectral bands) to cold optical benches (COB) located in two separate cryostats. The Observatoire de la Côte d'Azur is in charge of the WOP providing the spectral band separation, optical path equalization and modulation, pupil positioning, beam anamorphosis, beam commutation, and calibration. NOVA-ASTRON is in charge of the COB providing the functions of beam selection, reduction of thermal background emission, spatial filtering, pupil transfer, photometry and interferometry splitting, additional beam anamorphosis, spectral filtering, polarization selection, image dispersion, and image combination. The Max Planck Institut für Radio Astronomie is in charge of the operation and performance validation of the two detectors, a HAWAII-2RG from Teledyne for the L- and M- bands and a Raytheon AQUARIUS for the N-band. Both detectors are provided by ESO. The Max Planck Institut für Astronomie is in charge of the electronics and the cryostats for which the requirements on space limitations and vibration stability resulted on very specific and stringent decisions on the design. The integration and test of the COB: the two cryogenic systems, including the cold benches and the detectors, have been conducted at MPIA in parallel with the integration of the WOP at OCA. At the end of 2014, the complete instrument was integrated at OCA. Following this integration, a period of interface and alignment

  3. McDonald Observatory data on the comet Shoemaker-Levy 9 impacts on Jupiter and the resulting haze particles

    Science.gov (United States)

    Pryor, W. R.; Na, C. Y.; Cochran, A. L.; Cochran, W. D.; Barker, E. S.; Armosky, B. J.; Pulliam, C. E.

    1997-10-01

    Simultaneous light curves of the Comet Shoemaker-Levy 9 fragment R and V impacts were measured with the McDonald Observatory 2.7 m and 0.8 m telescopes, at wavelengths of 2.12 μm and 0.893 μm, respectively. The R impact was clearly detected at 2.12 μm, but not at 0.893 μm, leading to an upper limit on the "main event" temperature of 1300 K. The V impact was not detected. A possible detection of the U impact at 2.12 μm was recorded. CCD spectrophotometry of Jupiter was obtained with the McDonald 2.1 m telescope during the Shoemaker-Levy 9 impact period (17 July-23 July 1994 UT; Barker et al. (1994) Bull. Am. Astron. Soc.26, 1569). Spectra of Jupiter from 0.55 to 1.08 μm (10 Å resolution) were obtained using a long-slit CCD spectrograph (ES2), with a seeing-limited spatial resolution of about 1-2″. Impact regions were darker than neighboring non-impact regions by some 5-10% at all wavelengths except in the strong methane absorption bands (0.727, 0.864, and 0.890 μm) where the impact sites are brighter. Aerosol models of this spectral change are examined. The grey absorption observed is not typical of a population of particles much smaller than the wavelength. Neither is the similar haze brightening seen in two methane bands of similar strength at 0.727 and 0.864 μm. Our radiative transfer models of the H and E impact aites favor broad particle size distributions, with a mean particle radius = 0.25 μm and a log-normal size distribution of width b ≈ 0.6. A constant imaginary refractive index of 0.006 in this wavelength range provides an adequate spectral fit to the H data, while an index of 0.012 better fits the E data. Additional ES2 Jupiter spectra from June 1995 with both "blue" (0.31-0.58 μm) and "red" (0.55-1.08 μm) gratings were obtained. Blue spectra and images still show some evidence for residual impact haze opacity near the impact latitudes; red spectra and images do not. Apparently sedimentation of the larger particles in a broad initial size

  4. Tiempo e historia en el Islam

    Directory of Open Access Journals (Sweden)

    Viguera Molins, María Jesús

    2004-06-01

    Full Text Available As in other civilizations, time in Islam is one of the organizing principies of its concepts, representations and identity. The very emergence of this civilization, in 7thcentury Arabia, resulted in the establishment of an era, a calendar and an historical consciousness of its own. Within this specificity, there are different ways of understanding, living and feeling time and history: from the personal, subjective perspective to that of philosophers and astronomers to time in the organization of daily activities, and from history as a succession of reigns and dynasties. These different concepts and vantage points reflect the richness and complexity of a civilization that is currently spread across all five continents and more than 1400 years old since Hegira. Thus, for the "orthodox" Sunnites time is linear, whereas for the Shiites it is cyclical. Yet even the rationalization of history as a linear occurring is not free from a contested meaning relative to the political circumstances of the present, as a semantic analysis of the term dawla indicates.

    Como en otras civilizaciones, el tiempo en el Islam es uno de los principios organizativos de sus conceptos, sus representaciones y su identidad. El mismo surgimiento de esta civilización, en la Arabia del siglo VII de la Era Cristiana, supuso la constitución de una era, un calendario y una conciencia histórica propios. Dentro de esta especificidad, hay diferentes modos de entender, vivir y sentir el transcurso del tiempo y de la historia, desde una perspectiva personal y subjetiva a otra social y política en relación con reinados y dinastías, pasando por la misma organización de las actividades cotidianas y la producción filosófica y astronómica. Estas diferencias reflejan la riqueza y complejidad de una civilización que se extiende hoy por todos los continentes y sobrepasa los 1400 años desde la Hégira. Entre los sunníes u "ortodoxos", por ejemplo, el tiempo

  5. The Impact Rate on Solar System Satellites During the Late Heavy Bombardment

    Science.gov (United States)

    Dones, Henry C. Luke; Levison, H. F.

    2012-10-01

    Nimmo and Korycansky (2012; henceforth NK12) found that if the outer Solar System underwent a Late Heavy Bombardment (LHB) in the Nice model, the mass striking the icy satellites at speeds up to tens of km/s would have vaporized so much ice that moons such as Mimas, Enceladus, and Miranda would have been devolatilized. NK12's possible explanations of this apparent discrepancy with observations include (1) the mass influx was a factor of 10 less than that in the Nice model; (2) the mass distribution of the impactors was top-heavy, so that luck might have saved some of the moons from suffering large, vapor-removing impacts; or (3) the inner moons formed after the LHB. NK12 calculated the mass influx onto the satellites from the lunar impact rate estimated by Gomes et al. (2005) and scaling factors calculated by Zahnle et al. (1998, 2003; also see Barr and Canup 2010). Production of vapor in hypervelocity impacts was calculated from Kraus et al. (2011). We are calculating impact rates onto the giant planets and their moons in the context of the "Nice II" model (Levison et al. 2011). We find that NK12's assumed influx is an overestimate, by an amount we are quantifying. We will discuss implications for the origin of icy satellites. We thank the NASA Lunar Science Institute (http://lunarscience.nasa.gov/) for support. Barr, A.C., Canup, R.M., Nature Geoscience 3, 164-167 (2010). Gomes, R., Levison, H.F., Tsiganis, K., Morbidelli, A., Nature 435, 466-469 (2005). Kraus, R.G., Senft, L.E., Stewart, S.T., Icarus 214, 724-738 (2011). Levison, H.F., Morbidelli, A., Tsiganis, K., Nesvorný, D., Gomes, R., Astron. J. 142, article id. 152 (2011). Nimmo, F., Korycansky, D.G., Icarus 219, 508-510 (2012). Zahnle, K., Dones, L., Levison, H.F., Icarus 136, 202-222 (1998). Zahnle, K., Schenk, P., Levison, H.F., Dones, L., Icarus 163, 263-289 (2003).

  6. Impact of seeing and host galaxy into the analysis of photo-polarimetric microvariability in blazars. Case study of the nearby blazars 1ES 1959+650 and HB89 2201+044

    Science.gov (United States)

    Sosa, M. S.; von Essen, C.; Andruchow, I.; Cellone, S. A.

    2017-11-01

    Blazars, a type of Active Galactic Nuclei, present a particular orientation of their jets close to the line of sight. Their radiation is thus relativistically beamed, giving rise to extreme behaviors, specially strong variability on very short timescales (I.e., microvariability). Here we present simultaneous photometric and polarimetric observations of two relatively nearby blazars, 1ES 1959+650 and HB89 2201+044, that were obtained using the Calar Alto Faint Object Spectrograph mounted at the 2.2 m telescope in Calar Alto, Spain. An outstanding characteristic of these two blazars is the presence of well resolved host galaxies. This particular feature allows us to produce a study of their intrinsic polarization, a measurement of the polarization state of the galactic nucleus unaffected by the host galaxy. To carry out this work, we computed photometric fluxes from which we calculated the degree and orientation of the blazars polarization. Then, we analyzed the depolarizing effect introduced by the host galaxy with the main goal to recover the intrinsic polarization of the galactic nucleus, carefully taking into consideration the spurious polarimetric variability introduced by changes in seeing along the observing nights. We find that the two blazars do not present intra-night photo-polarimetric variability, although we do detect a significant inter-night variability. Comparing polarimetric values before and after accounting for the host galaxies, we observe a significant difference in the polarization degree of about 1% in the case of 1ES 1959+650, and 0.3% in the case of HB89 2201+044, thus evidencing the non-negligible impact introduced by the host galaxies. We note that this host galaxy effect depends on the waveband, and varies with changing seeing conditions, so it should be particularly considered when studying frequency-dependent polarization in blazars. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated

  7. El Real Instituto y Observatorio de la Armada

    Directory of Open Access Journals (Sweden)

    Boloix Carlos-Roca, Rafael C.

    2002-10-01

    Full Text Available Not available

    Desde 1753, en que fue creado por el insigne marino Jorge Juany Santacilia, el Real Instituto y Observatorio de la Armada (ROA ha sido el núcleo de la investigación científica de la Armada, manteniendo hoy día un reconocido prestigio tanto a nivel nacional como internacional. El autor de este artículo, director del ROA, a través de una síntesis descriptiva de la estructura orgánica del centro en cuatro Secciones (Efemérides, Astronomía, Geofísica, y Hora, nos introduce en la evolución histórica de esta institución y en la amplia gama de actividades que desarrolla en la actualidad, participando en numerosos proyectos y foros internacionales, y manteniendo relaciones de colaboración permanente con organismos científicos similares de diversos países. Sus publicaciones de efemérides astronómicas, sus trabajos en geomagnetismo, sismología, seguimiento de satélites, astrofísica, metrología, etc. etc., así como el hecho de ser el depositario del Patrón Nacional de la unidad de tiempo, son el exponente de que el ROA continúa siendo un centro científico en plena actividad y pujanza, y en no pocas ocasiones la voz de España en el concierto internacional de estas ramas del conocimiento y de la investigación. Finaliza el artículo con una breve referencia a la Escuela de Estudios Superiores, vinculada al ROA desde su creación y que continúa con sus cursos de «estudios mayores» manteniendo vivo el espíritu científico de la Armada, mediante la formación de un selecto núcleo de oficiales en las áreas de ciencias Físico-Matemáticas, Astronomía y Geofísica, y en la preparación para los cursos de Ingeniería.

  8. Tossing Out the Leftovers: The Fate of the Remains of Earth's Formation

    Science.gov (United States)

    Dones, L.; Levison, H. F.; Zahnle, K. J.

    1999-09-01

    Impact rates on the Moon and (presumably) Earth were orders of magnitude higher than they are now when the late lunar basins formed about 3900 Myr ago. Small bodies that remained in the inner solar system after the Earth and Moon formed have been suggested as possible basin-forming impactors (Wetherill 1975). As part of a study to determine whether various classes of small bodies might have produced the Late Heavy Bombardment, we have integrated the orbits of 200 test particles in the 0.7-1.3 AU region. The particles initially had circular orbits with zero inclination to the ecliptic. The integration included all the planets and was run for 100 Myr. 42% of the particles survived for 100 Myr; 23.5% hit Earth; 14% hit Venus; 14% hit the Sun; and 0.5% hit Mars. At late times the number, N, of particles that survive for time t goes as N = A - B log t, where A and B are constants (cf. Holman and Wisdom 1993, Evans and Tabachnik 1999). Using this law, we predict that about 10% of the particles would had survived to the time of the Late Heavy Bombardment, some 600 Myr after the solar system formed. Thus accretional leftovers are plausible impactors for producing the late lunar basins. However, if the Moon underwent a ''cataclysm,'' i.e., a sharp increase in the impact rate some 3900 Myr ago, some additional process, such as tidal disruption of a multi-100 km planetesimal by the Earth or Venus, would need to be invoked (Hartmann et al. 2000). Evans, N.W., and Tabachnik, S. (1999). Possible long-lived belts in the inner solar system. Nature 399, 41-43. Hartmann, W.K., Ryder, G., Dones, L., and Grinspoon, D. (2000). The time-dependent intense bombardment of the primordial Earth/Moon system. In Origin of the Earth and Moon (R. Canup and K. Righter, Eds.). Univ. Arizona Press and Lunar and Planetary Institute. Holman, M.J., and Wisdom, J. (1993). Dynamical stability in the outer solar system and the delivery of short period comets. Astron. J. 105, 1987-1999. Wetherill, G

  9. Investigation of the Hydantoin Monomer and its Interaction with Water Molecules

    Science.gov (United States)

    Gruet, Sébastien; Perez, Cristobal; Schnell, Melanie

    2017-06-01

    K., and Ohishi M., Astron. Astrophys., Forthcoming article (

  10. Descripción del coronógrafo a ser instalado en Argentina (MICA)

    Science.gov (United States)

    Stenborg, G.; Francile, C.; Schwenn, R.; Epple, A.; Rovira, M.

    El ``Coronógrafo de espejo para Argentina'' es un telescopio solar terrestre a ser colocado en el Observatorio Astronómico Félix Aguilar (El Leoncito), antes de finalizar 1996, como parte de un programa de ciencia bilateral entre Alemania y Argentina. Eclipses fotográficos de alta resolución han revelado que la corona solar es altamente estructurada y variable. De hecho, está contínuamente deformada y moldeada por los movimientos convectivos de los extremos de los arcos magnéticos en la fotosfera, estando, en muchas oportunidades, afectada por explosivas liberaciones de energía. MICA, en conjunción con otros telescopios solares espaciales y terrestres, tratará de contribuir al entendimiento de cuestiones fundamentales de la física solar. Entre ellas: cómo la corona está siendo calentada, dónde y cómo el viento solar es acelerado, qué causa los transitorios coronales, etc. Para ello investigará la distribución de los parámetros del plasma y su evolución con el tiempo, la estructura espacial de la corona en fina y gran escala, procesos que ocurren en los transitorios coronales y factores que los disparan, etc. Para responder a estas cuestiones MICA observará la atmósfera solar por sobre el limbo entre 1.1 y 2 radios solares aproximadamente, usando un nuevo tipo de sistema coronográfico que permite suprimir el brillo del disco solar suficientemente bien, tomando las imágenes con una cámara CCD de 1024x1024 pixels, codificada en 12 bits, pudiendo el mismo ser operado en forma remota. En la presente exposición describiremos las características del instrumento, cómo será controlado y qué esperamos observar basados en las imágenes obtenidas por los telescopios de similares características LASCO C1 a bordo del SOHO y PICO (ubicado en el Observatorio de Pic du Midi, Francia).

  11. La creación del mundo supralunar según Abraham Ibn Ezra: un estudio comparativo de sus dos comentarios a Génesis 1,14

    Directory of Open Access Journals (Sweden)

    Sela, Shlomo

    2003-06-01

    Full Text Available This article aims at elucidating Abraham Ibn Ezra's (ca. 1089 - ca. 1167 opinion about the creation of the supra-lunar world. A major and striking feature of Ibn Ezra's approach is that he did not find it convenient to address this issue, intimately related to the nature of the celestial bodies, in his astronomical or astrological treatises, but rather in his biblical commentaries. Therefore, we propose to concentrate our efforts on the meticulous study of the two commentaries which Ibn Ezra wrote on Genesis 1,14. As this verse focuses on the account of the creation of the heavenly bodies, we have assumed that the elusive Ibn Ezra could not have avoided revealing his view, or, at least, that we should have left some significant hints from which we may uncover his genuine opinion about the creation of the supra-lunar world.

    El propósito de este artículo es averiguar la opinión de Abraham Ibn Ezra (ca. 1089 - ca. 1167 sobre lo relacionado con la creación del mundo supralunar. Una característica fundamental dei modus operandi de Ibn Ezra es que, si buscamos información acerca de su opinión sobre la creación del mundo, tanto sublunar como supralunar, no la hallaremos en sus tratados científicos astronómicos o astrológicos, sino precisamente en sus comentarios bíblicos. Por lo tanto, la metodología más adecuada consistirá en concentrar nuestros esfuerzos en el estudio meticuloso de sus dos comentarios a Génesis 1,14. Dado que este verso bíblico tiene como objetivo principal el relato y la descripción de la creación de las luminarias, pensamos que en ambos comentarios Ibn Ezra no pudo haber eludido dar su verdadera opinión -o al menos dejar alguna pista significativa- sobre la creación del mundo supralunar.

  12. Inhomogeneous helicity effect in the solar angular-momentum transport

    Science.gov (United States)

    Yokoi, Nobumitsu

    2017-04-01

    Yoshizawa, A., "Statistical analysis of the effects of helicity in inhomogeneous turbulence," Phys. Fluids A, 5, 464-477 (1993). [2] Yokoi, N. and Brandenburg, A., "Large-scale flow generation by inhomogeneous helicity," Phys. Rev. E, 93, 033125-1-14 (2016). [3] Marino, R., Mininni, P., Rosenberg, D., and Pouquet, A., "Emergence of helicity in rotating stratified turbulence," Phys. Rev. E, 87, 033016-1-9 (2013). [4] Duarte, L. D. V., Wicht, J., Browning, M. K., and Gastine, T., "Helicity inversion in spherical convection as a means for equatorward dynamo wave propagation," Mon. Not. Roy. Astron. Soc. 456, 1708-1722 (2016).

  13. Exoplanets -New Results from Space and Ground-based Surveys

    Science.gov (United States)

    Udry, Stephane

    ). TandEM: Titan and Enceladus mission. Experimenta( Astron-omy, 23, 893-946. 3. Coustenis, A., Hirtzig, M., 2009. Cassini-Huygens results on Titan's surface. Research in Astronomy and Astrophysics 9, 249-268. 4. Coustenis et al., 2010, Titan trace gaseous composition from CIRS at the end of the Cassini-Huygens prime mission Icarus, in press. 5. Flasar, F. M., et al., 2005. Titan's atmospheric temperatures, winds, and composition. Science, 308, 975-978. 6. Fulchignoni, M., et al, 2005. In situ measurements of the physical characteristics of Titan's environment. Nature, 438, 785-791, doi:10.1038/nature04126. 7. Lebreton, J-P., Coustenis, A., et al., 2009. Results from the Huygens probe on Titan. Astron. Astrophys. Rev. 17, 149-179. 8. Tomasko, M. G., et al., 2005. Rain, winds and haze during the Huygens probe's descent to Titan's surface. Nature, 438, 765-778, doi: 10. 1038/nature04126.

  14. The Exploration of Titan and the Saturnian System

    Science.gov (United States)

    Coustenis, Athena

    ). TandEM: Titan and Enceladus mission. Experimenta( Astron-omy, 23, 893-946. 3. Coustenis, A., Hirtzig, M., 2009. Cassini-Huygens results on Titan's surface. Research in Astronomy and Astrophysics 9, 249-268. 4. Coustenis et al., 2010, Titan trace gaseous composition from CIRS at the end of the Cassini-Huygens prime mission Icarus, in press. 5. Flasar, F. M., et al., 2005. Titan's atmospheric temperatures, winds, and composition. Science, 308, 975-978. 6. Fulchignoni, M., et al, 2005. In situ measurements of the physical characteristics of Titan's environment. Nature, 438, 785-791, doi:10.1038/nature04126. 7. Lebreton, J-P., Coustenis, A., et al., 2009. Results from the Huygens probe on Titan. Astron. Astrophys. Rev. 17, 149-179. 8. Tomasko, M. G., et al., 2005. Rain, winds and haze during the Huygens probe's descent to Titan's surface. Nature, 438, 765-778, doi: 10. 1038/nature04126.

  15. Difficulties of First Years Elementary School Teachers with the Teaching of Astronomy. (Breton Title: Dificuldades de Professores dos Anos Iniciais do Ensino Fundamental em Relação ao Ensino da Astronomia. ) Dificultades de LOS Profesores de los Primeros Años de la Escuela Primaria en Relación a la Enseñanza de la Astronomía

    Science.gov (United States)

    Langhi, Rodolfo; Nardi, Roberto

    2005-12-01

    This paper reports Primary School teachers' discourses analysis about their difficulties related to the teaching of Astronomy. It reports partial data of a master's level research carried out in the last two years, named "An exploratory study for inserting Astronomy in primary school teachers' education" (LANGHI, 2004). The study took into consideration students' and teachers' common sense conceptions about astronomical phenomena, conceptual mistakes in textbooks, and Astronomy's suggestions given by the PCN (Parâmetros Curriculares Nacionais - The Brazilian National Curriculum Standards). The paper aims to characterize teachers' difficulties, in order to provide subsides to the implementation of an initial or continuing education program. This study is justified by the fact that courses plans like these only will be adapted to the teacher's (and students') reality, if there is a primary investigation about what the teachers really need to know about Astronomy. This fact was possible here by the enunciations interpretation of a teachers' sample using semi-structured interviews, according to discourse analysis procedures. The research outcomes show difficulties related to factors like: those of personal order, methodological, on teacher's formation, educational infrastructure and other related to information sources for educators. Este artigo, que relata as dificuldades de professores em relação ao ensino da Astronomia, faz parte de um estudo exploratório para a inserção da Astronomia na formação de professores dos anos iniciais do Ensino Fundamental. Esse estudo leva em consideração as concepções alternativas de alunos e professores sobre fenômenos astronômicos, os erros conceituais em livros didáticos e as sugestões de conteúdos de Astronomia constantes nos PCN (Parâmetros Curriculares Nacionais). Caracterizar as dificuldades dos professores é a questão central deste texto, apontando para o objetivo de contribuir com subsídios para um futuro

  16. Radio Telescopes "Save the Day," Produce Data on Titan's Winds

    Science.gov (United States)

    2005-02-01

    eventually provide a three-dimensional record of motion for the Huygens Probe during its mission at Titan. Huygens was built by the European Space Agency. The radio astronomy support of the Huygens mission is coordinated by JIVE and JPL and involves the National Radio Astronomy Observatory (Green Bank, WV and Socorro, NM), the Netherlands Foundation for Research in Astronomy (ASTRON, The Netherlands), the University of Bonn (Germany), Helsinki University of Technology (Espoo, Finland), the MERLIN National Facility (Jodrell Bank, UK), the Onsala Space Observatory (Sweden), the NASA Jet Propulsion Laboratory (Pasadena, CA), the CSIRO Australia Telescope National Facility (ATNF, Sydney, Australia), the University of Tasmania (Hobart, Australia), the National Astronomical Observatories of China, the Shanghai Astronomical Observatory (Shanghai and Urumqi, China) and the National Institute of Information and Communications Technologies (Kashima Space Research Center, Japan). The Joint Institute for VLBI in Europe is hosted by ASTRON and funded by the national research councils, national facilities and institutes of The Netherlands (NOW), the United Kingdom (PPARC), Italy (CNR), Sweden (Onsala Space Observatory, National Facility), Spain (IGN) and Germany (MPIfR). The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The Cassini-Huygens mission is a cooperation between NASA, ESA and ASI, the Italian space agency. The Jet Propulsion Laboratory (JPL), a division of the California Institute of Technology in Pasadena, is managing the mission for NASA's Office of Space Science, Washington DC. JPL designed, developed and assembled the Cassini orbiter while ESA operated the Huygens atmospheric probe. The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.

  17. The Understanding of Astronomy Concepts by Students from Basic Education of a Public School. (Spanish Title: El Entendimiento de Conceptos de Aastronmía Por Los Alumnos de Educación Básica en Una Escuela Pública.) O Entendimento de Conceitos de Astronomia Por Alunos da Educação Básica: O Caso de Uma Escola Pública Brasileira

    Science.gov (United States)

    Iria Machado, Daniel; dos Santos, Carlos

    2011-07-01

    We present the results obtained in a research on the comprehension of basic astronomical concepts, in which 561 students from fifth grade middle school to third grade high school of a public school of the city of Foz do Iguaçu (Brazil) took part. A test with 20 multiple-choice questions was applied to indentify the most common conceptions expressed by the students. This test was elaborated based on the literature about misconceptions and covered the following topics: the day-night cycle; the time zones; the seasons of the year; the phases of the Moon; the movement of the Moon; the apparent movement of the Sun in the celestial sphere; the eclipses; the dimensions and distances in the Universe; the brightness of the stars and its observation from Earth. Though a small progress was verified in the proportion of scientifically acceptable answers when comparing the eighth grade of middle school to the fifth, and the third grade of high school to the first, there was an overall predominance of alternative conceptions regarding most of the explored subjects, which persisted up to the last year of secondary school. The comparison to data found in this research made in other socio-cultural contexts revealed, in many aspects, similar notions and difficulties revealed by the students. Se presentan los resultados de una investigación sobre la comprensión de conceptos astronómicos básicos, en la cual participaron 561 estudiantes que cursaban entre el quinto grado de la enseñanza primaria y el tercer año de la enseñanza secundaria de una escuela pública de la ciudad de Foz do Iguaçu (Brasil). Se utilizó un test de 20 preguntas de opción múltiple para identificar las concepciones más comunes expresadas por los estudiantes. Este instrumento de recolección de datos se desarrolló en base a la literatura sobre las concepciones alternativas y trató los siguientes temas: el ciclo día-noche, los husos horarios, las estaciones del año, las fases de la Luna, el

  18. The Shadow of a Gnomon Along a Year: Routine Observations and Teaching of Apparent Motion of the Sun and the Four Seasons. (Spanish Title: La Sombra de un Gnomon lo Largo de un Año: Observaciones de Rutina y la Enseñanza del Movimiento Aparente del Sol y Las Cuatro Estaciones.) A Sombra de um Gnômon ao Longo de um Ano: Observações Rotineiras e o Ensino do Movimento Aparente do Sol E das Quatro Estações

    Science.gov (United States)

    Trogello, Anderson Giovani; Danhoni Neves, Marcos Cesar; de Carvalho Rutz da Silva, Sani

    2013-12-01

    , al solsticio de junio, al equinoccio de septiembre y al solsticio de diciembre. Además, se dictaron clases teóricas en la sala de aula. Estos métodos buscaron construir conceptos en torno al movimiento aparente del Sol y la sucesión de las estaciones. Teniendo en cuenta los resultados de las actividades se aplicó una evaluación cuyos datos demuestran la existencia de un aprendizaje deseado por los estudiantes en cuanto a: el reconocimiento de los puntos cardinales, la descripción del movimiento solar aparente y la aparición de las estaciones y su alternancia a partir de observaciones astronómicas visuales sin instrumentos. Muitas concepções alternativas são reconhecidas entre os diversos grupos de estudantes, em especial nos da educação básica. Dentre elas, o movimento aparente do Sol, por mais quotidiano que seja, proporciona variadas interpretações. Deste modo, observar e registrar o movimento dos astros na abóboda celeste é uma tarefa necessária ao ensino de Astronomia. O trabalho que ora se apresenta propõe a apresentação dos resultados da observação do movimento aparente do Sol por intermédio da marcação da sombra de um gnômon vertical por alunos de uma turma do sexto ano do ensino fundamental de uma escola do campo do Paraná. O projeto em si ocorreu em quatro etapas, em datas próximas do equinócio de março, do solstício de junho, do equinócio de setembro e do solstício de dezembro. Além disso, foram desenvolvidas aulas teóricas em sala de aula. Tais métodos buscaram construir conceitos em torno da movimentação aparente do Sol e da alternância das estações do ano. Diante dos resultados provenientes das atividades desenvolvidas foi aplicada uma avaliação e os dados demonstraram um aprendizado desejado dos alunos quanto: ao reconhecimento dos pontos cardeais; à descrição do movimento solar aparente e a ocorrência das estações do ano e sua alternância a partir de observações astronômicas a olho nu.

  19. Disciplines and Professors of Astronomy in Undergraduate Physics Teachers Formation Courses in Brazilian Universities. (Spanish Title: Disciplinas y Profesores de Astronomia en los Cursos de Licenciatura en Física en Las Universidades Brasileñas.) Disciplinas e Professores de Astronomia Nos Cursos de Licenciatura em Física das Universidades Brasileiras

    Science.gov (United States)

    Roberto, Artur Justiniano, Jr.; Reis, Thiago Henrique; dos Reis Germinaro, Daniel

    2014-12-01

    This article is the result of a research on basic training in Astronomy in physics degrees that performed the ENADE 2011 national examination. The objective was to identify whether there are disciplines of Astronomy in these courses, whether are mandatory or optional, its workload and when it is offered. The relationship between astronomers, physics degrees and disciplines of Astronomy was investigated. To perform this research we examined the results of ENADE 2011 and also the census of Brazilian Astronomical Society. As a result it is observed that in only 15% of the courses there is a mandatory subject of Astronomy, and therefore there is a high probability that 85% of physics teachers trained in 2011 have not had any discipline of Astronomy during their graduation. In addition, the data collected in this study shows a low number of members of SAB (Sociedade Astronômica Brasileira) among the surveyed courses. We have verified that the presence of astronomers in a given university does not imply to have a mandatory discipline of Astronomy in physics degrees at the same university. Este artículo es el resultado de una investigación sobre la formación básica en Astronomía en los cursos de Profesorado en Física que hicieron el examen nacional ENADE 2011. El objetivo del trabajo fue identificar se existen disciplinas de Astronomía en estos cursos, si son obligatorias u optativas, cuál es su carga horaria y el semestre en que son ofrecidas. Se investigó también la correlación entre astrónomos, los cursos de licenciatura en Física y las disciplinas de Astronomía. Para realizar esta investigación se utilizaron los datos del ENADE 2011 y también del censo de la Astronomía brasileña. Como resultado, se observó que en solo 15% de los cursos existe una disciplina obligatoria de Astronomía y que existe una grande probabilidad de que 85% de los profesores de Física formados en el año de 2011 no hayan cursado ninguna disciplina de Astronomía durante su

  20. Teaching of Astronomy: Scenarios of Teaching Practice in Elementary Schools. (Spanish Title: Enseñanza de la Astronomía: Semblanzas de la Práctica Docente en Educación Primaria.) Ensino de Astronomia: Cenários da Prática Docente no Ensino Fundamental

    Science.gov (United States)

    Marchi Gonzatti, Sônia Elisa; Spessatto De Maman, Andréia; Fernandes Borragini, Eliana; Kerber, Júlia Cristina; Haetinger, Werner

    2013-12-01

    atomización de los asuntos, aunque temas como movimientos de la Tierra y fenómenos astronómicos hayan sido citados por la mayoría de los participantes. En cuanto a las estrategias, se verifico que se emplean principalmente clases con el apoyo de recursos bidimensionales, como películas, textos, mapas y búsqueda en internet. Las principales dificultades fueron la falta de formación específica con respecto a los contenidos de Astronomía, y el nivel de abstracción exigido por los contenidos. De modo general, esos indicadores convergen para los resultados ya encontrados en otros estudios, en el que las deficiencias de la formación inicial de los profesores, o incluso su ausencia, dificulta el adecuado abordaje de la Astronomía en las clases. Neste trabalho são apresentados os principais resultados de uma investigação realizada no campo da Educação em Astronomia, com professores do ensino fundamental de duas regiões do Rio Grande do Sul. O objetivo do estudo foi caracterizar o cenário regional do ensino de Astronomia, estabelecendo um comparativo com o cenário nacional. Esse estudo abordou três questões: identificar os principais temas de astronomia trabalhados em sala de aula, as estratégias metodológicas e quais as dificuldades apresentadas pelos professores ao desenvolver sua prática. Quanto aos conteúdos, encontrouse uma pulverização dos assuntos abordados, embora temas como movimentos da Terra e fenômenos astronômicos tenham sido citados pela maioria dos participantes. Sobre estratégias, são utilizadas principalmente aulas com apoio de recursos bidimensionais, como filmes, textos, mapas e pesquisa na internet. As principais dificuldades foram: falta de formação específica em relação a conteúdos de Astronomia; nível de abstração dos conteúdos, que dificultam sua compreensão, tanto pelos alunos quanto pelos próprios professores. De maneira geral, esses indicadores convergem para resultados já encontrados em outros estudos que

  1. Development of Educational Resources to Include the Teaching of Astronomy in the First Years of the Basic Education. (Spanish Title: Desarrollo de Recursos Pedagógicos Para Incluir la Enseñanza de la Astronomía en los Primeros Años de la Educación Básica.) Desenvolvimento de Recursos Pedagógicos Para Inserir o Ensino de Astronomia nas Séries Iniciais do Ensino Fundamental

    Science.gov (United States)

    da Silva Morett, Samara; de Oliveira Souza, Marcelo

    2010-07-01

    ía y la vida cotidiana de los estudiantes. La inclusión de la astronomía en la escuela primaria es una manera de demostrar a los estudiantes cómo este campo está presente de forma activa en su vida cotidiana. Las clases que participan en el proyecto participaron en un estudio con el objetivo de proporcionar información a los conocimientos previos que tenían sobre los temas de la astronomía que se examinaron durante el proyecto. Con los experimentos realizados, y la ayuda de las nuevas tecnologías, conceptos astronómicos fueron presentados a los estudiantes de 4to y 5to año de la educación básica de una escuela municipal de Campos dos Goytacazes (RJ). Después de las presentaciones nuevos datos fueran colectados y se han llevado a cabo con el fin de verificar el nivel de aprendizaje alcanzado y se observó que el método utilizado fue una herramienta importante para ayudar al proceso de enseñanza y aprendizaje. El proyecto logró resultados satisfactorios. Neste trabalho será apresentado o desenvolvimento de recursos pedagógicos para a apresentação de conceitos de astronomia nas séries iniciais do ensino fundamental. Este material é composto por apresentações realizadas com o uso de novos recursos tecnológicos, pela fabricação de experimentos e a discussão de curiosidades relativas a esta área de conhecimento. Os experimentos foram construídos com material de baixo custo com o objetivo de permitir que os alunos envolvidos pudessem refazê-los em outras ocasiões. O material apresentado busca enfatizar a relação entre a astronomia e o cotidiano dos alunos. A inclusão da astronomia no ensino fundamental e uma forma de demonstrar aoestudante como esta área está presente de forma ativa em seu cotidiano. As turmas envolvidas no projeto participaram de uma pesquisa com o objetivo de obter dados relativos ao conhecimento prévio que possuíam sobre os tópicos de astronomia que foram considerados no decorrer do projeto. Com os experimentos

  2. Análise Temporal da Coma de CO+ no Cometa P/Halley

    Science.gov (United States)

    Voelzke, M. R.; Schlosser, W.; Schmidt-Kaler, Th.

    1995-08-01

    Observações fotográficas e fotoelétricas da coma de gás ionizado do cometa P/Halley a nível de CO+ em 4250 angstroms fizeram parte do programa de Monitoramento do Halley desenvolvido pela Universidade de Bochum (Ruhr-Universitaet Bochum) na Alemanha, realizado de 17 de fevereiro a 17 de abril de 1986 no European Southern Observatory (ESO) em La Silla (Chile). Nesta faixa espectral é possível observar a contínua formação, bem como o movimento e expansão das estruturas de plasma. Para observar a morfologia destas estruturas foram analisadas 32 placas fotográficas de CO+ (placas de vidro) do cometa P/Halley. Tais placas possuem um campo de visão de 28,6 por 28,6 graus sendo obtidas entre 29 de março e 17 de abril de 1986 com tempos de exposição entre 20 e 120 minutos. Todas as placas foram digitadas com o auxílio de um microdensitômetro PDS 2020 GM (Photometric Data System) do Instituto Astronómico da Westfaelischen Wilhelms-Universitaet em Muenster, Alemanha (um pixel = 25 por 25 micrômetros correspondendo aproximadamente a 46,88 por 46,88 segundos de arco). Após a digitação os dados foram reduzidos à intensidades relativas, sendo que os posssíveis de calibração também foram reduzidos à intensidades absolutas, expressas em termos de densidade colunar utilizando-se dos sistemas de tratamento de imagens MIDAS (Munich Image Data Analysis System; ESO - Image Processing Group, 1988) e IHAP (Image Handling And Processing; Middleburg, 1983). Com o auxílio do método de teta mínimo de Stellingwerf (Stellingwerf, 1978) obteve-se um período de 2,22 +/- 0,09 dias a partir da análise de estruturas na coma de plasma através da subtração de imagens subsequentes. Este método foi comparado com o método de Fourier. Provavelmente exista um segundo ciclo com período aproximado de 3,6 dias. A idéia de subtrair imagens subsequentes é devido ao fato de que os efeitos de rotação são apenas 10% dos fenômenos de distribuição gasosa. Portanto as

  3. Twenty-four-week effects of liraglutide on body composition, adherence to appetite, and lipid profile in overweight and obese patients with type 2 diabetes mellitus

    Directory of Open Access Journals (Sweden)

    Rondanelli M

    2016-03-01

    Full Text Available Mariangela Rondanelli,1 Simone Perna,1 Paolo Astrone,2 Annalisa Grugnetti,2 Sebastiano Bruno Solerte,2 Davide Guido3,4 1Endocrinology and Nutrition Unit, Section of Human Nutrition, Department of Public Health, Experimental and Forensic Medicine, Agency for Elderly People Services, Santa Margherita Hospital, University of Pavia, Pavia, Italy; 2Section of Geriatrics and Gerontology, Department of Internal Medicine, Agency for Elderly People Services, Santa Margherita Hospital, University of Pavia, Pavia, Italy; 3Medical and Genomics Statistics Unit, Department of Brain and Behavioral Sciences, University of Pavia, Pavia, Italy; 4Biostatistics and Clinical Epidemiology Unit, Department of Public Health, Experimental and Forensic Medicine, University of Pavia, Pavia, Italy Background: Liraglutide has well-known effects on glucose patterns. However, its several other metabolic properties are still controversial. Given this background, the aims of the present study are to evaluate the effects of 24-week liraglutide treatment on body composition, appetite, and lipid profile in overweight and obese type 2 diabetes mellitus (T2DM patients. Methods: A cohort study was carried out on overweight and obese T2DM patients with glycosylated hemoglobin A1c equal to 6% (42 mmol/mol-10% (86 mmol/mol, under a 3-month treatment (at least with maximal dose of metformin as stable regime, by adding liraglutide at doses up to 3 mg/d. Body composition markers were measured by dual-energy X-ray densitometry at baseline and after 24 weeks of liraglutide treatment. Glucose control was monitored by glucose, glycosylated hemoglobin A1c, insulin, and homeostasis model assessment. Finally, the appetite sensation and plasma lipids were also evaluated. Results: Twenty-eight subjects (male/female: 16/12, mean age: 58.75±9.33 years, body mass index: 34.13±5.46 kg/m2 were evaluated. Accounting for the adjustment for age, sex, and duration of diabetes, we noted significant

  4. Aqueous processing of organic compounds in carbonaceous asteroids

    Science.gov (United States)

    Trigo-Rodríguez, Josep Maria; Rimola, Albert; Martins, Zita

    2015-04-01

    A (2002) Clay mineral-organic matter relationships in the early solar system. Meteorit Planet Sci 37:1829-1833. Rimola A, Costa D, Sodupe M, Lambert JF, Ugliengo P (2013) Silica surface features and their role in the adsorption of biomolecules: computational modeling and experiments. Chem Rev 113:4216-4313. Rimola A, Sodupe M, Ugliengo P (2007) Aluminosilicate as promoters for peptide bond formation: an assessment of Bernal's hypothesis by ab initio methods. J Am Chem soc 129:8333-8344 Trigo-Rodríguez JM, Moyano-Cambero CE, Llorca J, Formasier S, Barucci MA, Belskaya I, Martins Z, Rivkin AS, Dotto E, Madiedo JM, Alonso-Azcárate J (2014) UV to far-IR reflectance spectra of carbonaceous chondrites - I. Implications for remote characterization of dark primitive asteroids targeted by sample-return missions. Mon Not R Astron Soc 437:227-240. Trigo-Rodríguez JM, Alonso-Azcárate J, Abad MM, Lee MR (2015) Ultra high resolution Transmission Electron Microscopy of matrix mineral grains in CM chondrites: preaccretionary or parent body aqueous processing? LPI constribution, 46th LPSC, abstract #1198.

  5. Estado Vital de la Materia. Su origen, su evolución y su futuro.

    Directory of Open Access Journals (Sweden)

    J. Hernando Ordoñez

    2001-04-01

    Full Text Available

    En este artlculo se hacen algunas observaciones sobre un estado de la materia (estado vital, propuesto para reemplazar el de materia viva, que se usa habitualmente.

    La materia en estado vital se organiza por una fuerza interna, que podríamos calificar como inteligente, que hace que los átomos se orienten y se organicen con determinada finalidad para fabricar células, para modelar órganos y, éstos, para culminar su obra integrándose con la armonía más admirable, para constituirse en organismos ya sea vegetales o animales.

    Los planetas no tienen materia en estado vital; son masas que giran y giran, aparentemente sin finalidad conocida. En cambio, en nuestro planeta una buena parte de su masa adquirió vida, lo que llamamos biomasa, que abarca todos los organismos vivos, tanto vegetales como animales, en una proporción tal que si se pudiera calcular su peso nos daría cifras astronómicas.

    Sobre el futuro de nuestro sol los científicos predicen que en los próximos 1.100 millones de años aumentará su luminosidad en un 10%. Esto sobre calentará a la Tierra como consecuencia de un severo efecto de invernadero. El agua de los mares y océanos hervirá y la vida en el planeta se extinguirá.

    El universo está constituido por energía y materia, que pueden transformarse la una en la otra. La energía se presenta en varias fases, entre ellas, en la energía eléctrica, la luz y el calor, cuya naturaleza íntima nos es tan desconocida. La materia también está en varios estados: sólido, líquido, gaseoso, iónico, molecular y coloidal.

    En el presente estudio intento hacer algunas observaciones sobre otro estado de la materia, que he denominado estado vital, nombre que propongo para reemplazar el de materia viva, que se usa habitualmente. Par hacerlo me baso en una consideración elemental: los átomos que integran la biomasa terrestre son los mismos que constituyen la materia inerte, no están vivos. En

  6. Mercury: a prediction for bulk chemical composition and internal structure in readiness for new MESSENGER data

    Science.gov (United States)

    Prentice, A. J.

    2008-12-01

    The MESSENGER spacecraft has confirmed that Mercury's magnetic field is dominantly dipolar and due to an active dynamo in a molten outer core (Solomon et al, 2008 Science 321 59). An energy source is needed to maintain this dynamo. Either liquid iron is freezing at the surface of an inner solid core (as proposed here) or solid iron is precipitating within an outer sulphur-rich core (Chen et al, 2008 GRL 35 L07201). If the outer core does not contain sulphur and consists solely of pure metal (Fe, Ni, Cr,..), then an active dynamo is inconsistent with previous numerical models for the radiogenic thermal evolution of the planet. Those earlier models found that the present temperature at the core/mantle boundary (CMB) is ~ 500 K below the melting temperature of metal ~ 2030 K for a CMB pressure of 70 kbar. The earlier calculations were based on low lunar abundances of U and Th. Here I present a new model for the bulk chemical composition, thermal evolution and current internal structure of Mercury. The model is based on the modern Laplacian theory of solar system origin (Prentice, 1978 Moon Planets 19 341; 2001 Earth Moon & Planets 87 11; 2006 Publ. Astron. Soc. Aust. (PASA) 23 1; 2008 - URL below). A key feature of this theory is that the planets formed from a concentric system of gas rings (n = 0, 1, 2,..) that were shed by the contracting protosolar cloud. The temperatures Tn of the rings scale with mean orbital radius Rn closely as Tn ~ Rn-0.9. Mercury plays a crucial role in calibrating this relationship because of a condensation process of metal/silicate fractionation (Lewis, 1972 EPSL 15 286). Choosing Tn ~ 1630 K for mean orbit gas ring pressure of 0.17 bar, the condensate consists mostly of Fe-Ni-Cr (mass fraction 0.671), gehlenite (0.190) and Mg-silicates (0.081). It has mean density 5.30 g/cm3. Na, K and S are absent. The mass fractions of U and Th, namely 5.66 × 10-8 & 2.08 × 10-7, are a factor of 4.3 times greater than those of the proto-Earth condensate

  7. Modelos MLG e MAG para análise da associação entre poluição atmosférica e marcadores de morbi-mortalidade: uma introdução baseada em dados da cidade de São Paulo GLM and GAM model for analyzing the association between atmospheric pollution and morbidity-mortality markers: an introduction based on data from the city of São Paulo

    Directory of Open Access Journals (Sweden)

    Gleice Margarete de Souza Conceição

    2001-11-01

    Full Text Available Este estudo, descreve e compara duas classes de modelos - os Modelos Lineares Generalizados (MLG e os Modelos Aditivos Generalizados (MAG - que podem ser utilizadas para avaliar a associação entre poluição atmosférica e marcadores de morbi-mortalidade. Enfoca os MAG como uma alternativa para a modelagem de relações não lineares não especificadas, e mostra que essa classe de modelos constitui uma boa opção para representar tanto a sazonalidade quanto a relação entre o desfecho e as variáveis meteorológicas. Como exemplo de aplicação é avaliada a associação entre mortalidade em idosos e poluição atmosférica na cidade de São Paulo no período de 1994 a 1997. Os dados de mortalidade foram obtidos do Programa de Aprimoramento das Informações de Mortalidade (PRO-AIM e as concentrações diárias de poluentes (PM10, SO2, CO, e ozônio foram obtidas da Companhia de Tecnologia de Saneamento Ambiental (CETESB. Informações acerca da temperatura e umidade relativa do ar foram obtidas do Instituto Astronômico e Geofísico da Universidade de São Paulo (IAG-USP. As duas classes de modelos produziram resultados coerentes, mas os modelos estatisticamente mais sofisticados tiveram mais poder para detectar efeitos significantes. Foram observadas associações entre mortalidade e os níveis de CO, SO2 e, em menor escala, PM10. As associações observadas foram dose-dependente e evidentes após um curto período de exposição.In this study, we have described and compared two classes of models - the Generalized Linear Models (GLM and the Generalized Additive Models (GAM _ which can be used to evaluate the association between atmospheric pollution and morbidity and mortality counts. We consider GAM as an alternative for modeling unspecific nonlinear relationships, and show that this class of models constitute a good option to represent both seasonality and the relation between the outcome and the meteorological variables. As an

  8. Astrodynamical Space Test of Relativity using Optical Devices I (ASTROD I)—a class-M fundamental physics mission proposal for cosmic vision 2015-2025: 2010 Update

    Science.gov (United States)

    Braxmaier, Claus; Dittus, Hansjörg; Foulon, Bernard; Göklü, Ertan; Grimani, Catia; Guo, Jian; Herrmann, Sven; Lämmerzahl, Claus; Ni, Wei-Tou; Peters, Achim; Rievers, Benny; Samain, Étienne; Selig, Hanns; Shaul, Diana; Svehla, Drazen; Touboul, Pierre; Wang, Gang; Wu, An-Ming; Zakharov, Alexander F.

    2012-10-01

    dedicated to probe gravitational waves at frequencies below the LISA bandwidth to 100 nHz and to detect solar g-mode oscillations. In the third phase (Super-ASTROD), larger orbits could be implemented to map the outer solar system and to probe primordial gravitational-waves at frequencies below the ASTROD bandwidth. This paper on ASTROD I is based on our 2010 proposal submitted for the ESA call for class-M mission proposals, and is a sequel and an update to our previous paper (Appouchaux et al., Exp Astron 23:491-527, 2009; designated as Paper I) which was based on our last proposal submitted for the 2007 ESA call. In this paper, we present our orbit selection with one Venus swing-by together with orbit simulation. In Paper I, our orbit choice is with two Venus swing-bys. The present choice takes shorter time (about 250 days) to reach the opposite side of the Sun. We also present a preliminary design of the optical bench, and elaborate on the solar physics goals with the radiation monitor payload. We discuss telescope size, trade-offs of drag-free sensitivities, thermal issues and present an outlook.

  9. Nuevo algoritmo de detección y corrección de píxeles anómalos en imágenes A new algorithm for detecting and correcting bad pixels in infrared images

    Directory of Open Access Journals (Sweden)

    Restrepo Gir��n Andrés David

    2010-08-01

    Full Text Available Se expone un nuevo algoritmo de procesamiento de imágenes para detectar y corregir píxeles anómalos que resalten de manera individual entre sus vecinos en imágenes de una secuencia térmica obtenida a partir de un procedimiento de termografía activa, sin afectar la apariencia global de cada imagen, como ocurre al emplear una estrategia clásica de filtrado espacial. Como resultado principal de este filtrado selectivo, se detectan y reemplazan en un alto porcentaje aquellos píxeles defectuosos de fabricación o por el uso continuo del dispositivo CCD de la cámara infrarroja, lo cual re- duce el riesgo de malas interpretaciones en el análisis posterior. Para el desarrollo y prueba del algoritmo propuesto se utilizaron secuencias de video tomadas con una cámara Cincinnati Electronics de indio-antimonio (InSb para inspeccionar láminas de CFRP (plástico reforzado con fibra de carbono mediante la técnica de termografía activa. Los resultados del algoritmo se comparan con una lista de píxeles defectuosos dada por el fabricante de la cámara, arrojando un porcentaje de coincidencia de alrededor del 70%. El presente trabajo toma relevancia al considerar que en la literatura científica se encuentran muy pocos estudios en este campo, centrándose la mayoría en el preprocesamiento de imágenes astronómicas; además, en Colombia se está en una etapa de introducción creciente de técnicas de evaluación no destructiva por termografía (ENDT en amplios sectores industriales que incluyen generación y transmisión de energía, in- genios azucareros y aeronáutica militar, entre otros.An image processing algorithm detects and replaces abnormal pixels individually, highlighting them amongst their neighbours in a sequence of thermal images without affecting overall texture, like classical filtering does. Bad pixels from manufacture or constant use of a CCD device in an IR camera are thus detected and replaced with a very good success rate

  10. Redetermination of the space weathering rate using spectra of Iannini asteroid family members

    Science.gov (United States)

    Willman, Mark; Jedicke, Robert; Nesvorný, David; Moskovitz, Nicholas; Ivezić, Željko; Fevig, Ronald

    2008-06-01

    We have obtained moderate S/N (˜85) spectra at a realized resolution of R˜100 for 11 members of the Iannini family, until recently the youngest known family at under 5 million years of age [Nesvorný, D., Bottke, W.F., Levison, H.F., Dones, L., 2003. Astrophys. J. 591, 486-497, 720-771]. The spectra were acquired using the Echellette Spectrograph and Imager in its low-resolution prism mode on the Keck II telescope. The family members belong to the S-complex of asteroids with perhaps some K class members. The Iannini family members' average spectral slope, defined as the slope of the best-fit line constrained to pivot about 1 at 550 nm, is (0.30±0.04)/μm, matching the (0.26±0.03)/μm reported by Jedicke et al. [Jedicke, R., Nesvorný, D., Whiteley, R.J., Ivezić, Ž., Jurić, M., 2004. Nature 429, 275-277] using SDSS [Ivezić, Ž., Jurić, M., Lupton, R.H., Tabachnik, S., Quinn, T., 2002. In: Tyson, J.A., Wolff, S. (Eds.), Survey and Other Telescope Technologies and Discoveries. In: Proc. SPIE, vol. 4836. SPIE, Bellingham, pp. 98-103] color photometry. Using our spectra for this family as well as new observations of Karin family members [Vernazza, P., Birlan, M., Rossi, A., Dotto, E., Nesvorný, D., Brunetto, R., Fornasier, S., Fulchignoni, M., Renner, S., 2006. Astron. Astrophys. 460, 945-951] and new classifications of some older families we have revised the space weathering rate of S-complex asteroids originally determined by Jedicke et al. [Jedicke, R., Nesvorný, D., Whiteley, R.J., Ivezić, Ž., Jurić, M., 2004. Nature 429, 275-277]. Following Jedicke et al. [Jedicke, R., Nesvorný, D., Whiteley, R.J., Ivezić, Ž., Jurić, M., 2004. Nature 429, 275-277] we parameterize the space weathering rate of the principal component color of the spectrum ( PC), which is correlated with the spectral slope, as PC(t)=PC(0)+ΔPC[1-exp]. Our revised rate suggests that the characteristic time scale for space weathering is τ=570±220 Myr and that new S-complex clusters

  11. Emergence of Habitable Environments in Icy World Interiors

    Science.gov (United States)

    Neveu, Marc

    2016-07-01

    separation method that takes advantage of the density contrast between cells and sediment and preserves cellular elemental contents [11]. Using this method, I showed that in spite of the tremendous physical, chemical, and taxonomic diversity of Yellowstone hot springs, the composition of microorganisms there is surprisingly ordinary [12]. This suggests the existence of a stoichiometric envelope common to all life as we know it. Thus, future planetary investigations could use elemental fingerprints to assess the astrobiological potential of hydrothermal settings beyond Earth. References: [1] US National Research Council (2011)Vision & Voyages in the Decade 2013-2022. [2] Hussmann et al. (2006) Icarus 185, 258-273. [3] Desch et al. (2009) Icarus 202, 694-714. [4] Neveu et al. (2015) JGR 120, 123-154. [5] Neveu & Rhoden, in prep. [6] De Sanctis et al. (2015) Nature 528, 241-244. [7] Hsu et al. (2015) Nature 519, 207-210. [8] Wasson & Kallemeyn (1988) Phil Trans R Soc London A 325, 535-544. [9] Mumma & Charnley (2011) Annu Rev Astron Astrophys 49, 471. [10] Neveu et al., in revision. [11] Neveu et al. (2014) Limn Oceanogr 12, 519-529. [12] Neveu et al. (2016) Geobiology 14, 33-53.

  12. Comparison of Regression and Neural Networks Models to Estimate Solar Radiation Comparación de Regresión y Modelos de Redes Neuronales para Estimar la Radiación Solar

    Directory of Open Access Journals (Sweden)

    Mónica Bocco

    2010-09-01

    ón multicapa, para estimar la radiación solar global diaria y comparar la eficiencia de los mismos en su aplicación para una región de la Provincia de Salta, Argentina. Se utilizaron datos de heliofanía relativa, temperaturas máxima y mínima, precipitación, precipitación binaria y radiación solar astronómica provistos por la Estación Experimental Salta, Instituto Nacional de Tecnología Agropecuaria (INTA, Argentina, correspondientes al período 1996-2002. Tanto para los modelos de redes neuronales como para las regresiones lineales se consideraron tres alternativas de combinaciones de los parámetros meteorológicos, obteniéndose buenos resultados con ambas metodologías de predicción, con valores de la raíz del error cuadrático medio variando desde 1.99 a 1.66 MJ m-2 d-1 y coeficientes de correlación de 0.88 a 0.92. Se concluye que ambos, los modelos de redes neuronales y las regresiones lineales, pueden ser usados para predecir en forma adecuada la radiación solar global diaria; si bien las redes neuronales produjeron mejores resultados.

  13. HD 50844: a new look at δ Scuti stars from CoRoT space photometry

    Science.gov (United States)

    Poretti, E.; Michel, E.; Garrido, R.; Lefèvre, L.; Mantegazza, L.; Rainer, M.; Rodríguez, E.; Uytterhoeven, K.; Amado, P. J.; Martín-Ruiz, S.; Moya, A.; Niemczura, E.; Suárez, J. C.; Zima, W.; Baglin, A.; Auvergne, M.; Baudin, F.; Catala, C.; Samadi, R.; Alvarez, M.; Mathias, P.; Paparò, M.; Pápics, P.; Plachy, E.

    2009-10-01

    , Belgium, Brazil, Germany, and Spain. This work is based on ground-based observations made with ESO telescopes at the La Silla Observatory under the ESO Large Programme LP178.D-0361 and on data collected at the Observatorio de Sierra Nevada (Spain), at the Observatorio Astronómico Nacional San Pedro Mártir (Mexico), and at the Piszkéstetö Mountain Station of Konkoly Observatory (Hungary). Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/85 Current address: Laboratoire AIM, CEA/DSM CNRS Université Paris Diderot, CEA, IRFU, SAp, centre de Saclay, 91191 Gif-sur-Yvette, France.

  14. Direito à Educação no Brasil e dívida educacional: e se o povo cobrasse? Right to education in Brazil and the educational debt: what if the people actually demanded it?

    Directory of Open Access Journals (Sweden)

    Alceu Ravanello Ferraro

    2008-08-01

    Full Text Available Inicia-se tratando do direito à Educação no quadro dos direitos fundamentais da pessoa humana e do conceito de dívida educacional que decorre da não-realização do direito público subjetivo de cada cidadão e cidadã à Educação Fundamental completa, conforme estabelecido na Constituição de 1988. Utilizando como parâmetro a informação censitária sobre o número de anos de estudo concluídos com aprovação levantados no Censo 2000, estima-se que, nesse ano, o Estado brasileiro devia, aos 119,6 milhões de pessoas de 15 anos ou mais, a astronômica cifra de 325,5 milhões de anos de estudo não realizados na idade própria - uma média de quase três anos por pessoa. São projetados também os investimentos necessários em termos de professores e salas de aula/turno-ano para o resgate da dívida. Mostra-se ainda que a dívida estimada com base na Pesquisa Nacional por Amostra de Domicílios 2005 (316,4 milhões de anos de estudo devidos representa uma diminuição muito pequena em relação ao Censo 2000. Por fim, aborda-se a questão dos atores ou agentes da efetividade do direito à Educação e dos instrumentos de exigibilidade que a legislação põe à disposição desses mesmos agentes. Conclui-se afirmando que está posto aí, para a sociedade em geral e para educadores e educadoras em particular, o grande desafio de despertar nas pessoas humildes a consciência de que elas efetivamente têm direito à Educação e de que dispõem de meios para cobrar do Estado esse direito.We start by considering the right to Education within the framework of the fundamental human rights, and the ensuing concept of educational debt, which follows from the failure to enforce the subjective public right of each citizen to a complete Fundamental Education as established by the 1988 Brazilian Constitution. Based on the 2000 census information on the number of years of schooling successfully concluded, we estimate that in that year the Brazilian

  15. The dependence of oxygen and nitrogen abundances on stellar mass from the CALIFA survey

    Science.gov (United States)

    Pérez-Montero, E.; García-Benito, R.; Vílchez, J. M.; Sánchez, S. F.; Kehrig, C.; Husemann, B.; Duarte Puertas, S.; Iglesias-Páramo, J.; Galbany, L.; Mollá, M.; Walcher, C. J.; Ascasíbar, Y.; González Delgado, R. M.; Marino, R. A.; Masegosa, J.; Pérez, E.; Rosales-Ortega, F. F.; Sánchez-Blázquez, P.; Bland-Hawthorn, J.; Bomans, D.; López-Sánchez, Á. R.; Ziegler, B.; Califa Collaboration

    2016-10-01

    explain the presence of inverted gradients in this sample, and there is no dependence between the average slopes and the presence of a bar. The relation between the resulting O/H and N/O linear fittings at the effective radius is much tighter (correlation coefficient ρs = 0.80) than between O/H and N/O slopes (ρs = 0.39) or for O/H and N/O in the individual H II regions (ρs = 0.37). These O/H and N/O values at the effective radius also correlate very tightly (less than 0.03 dex of dispersion) with total luminosity and stellar mass. The relation with other integrated properties, such as star formation rate, colour, or morphology, can be understood only in light of the found relation with mass. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).Full Table 1 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/595/A62

  16. Identificación de los miembros del cúmulo NGC 2516

    Science.gov (United States)

    de Elía, G. C.; Orellana, R. B.

    El cúmulo abierto NGC 2516 (α = 7h 58m y δ = -60o 45') tiene una edad de, aproximadamente, 150 Myr. El análisis de este sistema es particularmente importante en el Hemisferio Sur debido a su abundancia de estrellas peculiares y muy estudiado aplicando técnicas fotométricas, pero muy poco analizado desde el punto de vista astrométrico. A partir de una placa obtenida en el Observatorio Astronómico de La Plata y observaciones más actuales, nos hemos abocado al estudio de los movimientos propios de este cúmulo con el fin de determinar la pertenencia al mismo de las estrellas del campo de dicho cúmulo. Luego de llevar a cabo la determinación de los movimientos propios de todas las estrellas a partir de las posiciones obtenidas de la placa existente en el Observatorio de La Plata de 1914 y leídas con la MAMA en París, las observaciones realizadas con el círculo meridiano de San Fernando que se encuentra en el Observatorio Félix Aguilar de San Juan y las posiciones existentes en los catálogos AC 2000, Tycho, USNO y UCAC, programamos el método de Vasilevsky y Sanders para determinar la pertenencia de las estrellas de la región al cúmulo en cuestión. En un paso posterior, se realizó una modificación al método anterior para la determinación de los miembros. En esta modificación se consideró la densidad de las estrellas del cúmulo y la densidad de estrellas de campo. Esto permitió evaluar la pertenencia, no sólo a partir del movimiento propio de las estrellas, sino también a partir de la posición de las mismas con respecto al centro del cúmulo. También se consideró la dependencia de los parámetros con la magnitud. Los resultados así obtenidos fueron comparados con otras investigaciones de movimientos propios de la región del cúmulo. El movimiento propio absoluto del cúmulo fue comparado con el obtenido a partir de los catálogos estelares. Se encontró que los resultados coincidían para estrellas brillantes (magnitud más brillante que

  17. Identification of Saturn-driven bending waves in Saturn's inner C ring

    Science.gov (United States)

    French, Richard; Colwell, Joshua; Nicholson, Phillip; Marouf, Essam; McGhee-French, Colleen; Hedman, Matthew

    2016-07-01

    Saturn's C ring is host to more than a dozen wavelike features whose detailed nature has been a mystery since their discovery in high-resolution Voyager radio occultations of the rings. Rosen et al. (1991 Icarus 93, 25) enumerated several of these, and the list was augmented by Baillié et al. (2011 Icarus 216, 292), based on a detailed analysis of Cassini UVIS stellar occultation profiles. Recently, Hedman and Nicholson (2013 Astron. J. 146, 12; 2014 MNRAS 444, 1369) were able to identify the wavenumbers and pattern speeds for several of the waves. They showed that several Outer Lindblad Resonances (OLR) density waves had properties that were in general quite consistent with the predictions of Marley and Porco (1993 Icarus, 106, 508) and Marley (2014 Icarus, 234, 194) that Saturn's acoustic oscillations had pattern speeds with corresponding resonance radii in the C ring. Hedman and Nicholson also identified a set of Inner Lindblad Resonance density waves with pattern speeds very close to Saturn's rotation period. Finally, French et al. (2016 Icarus, in press) identified an inward-propagating m=2 wave in the Maxwell Ringlet. These new identifications ushered in the field of Kronoseismology -- the probing of the nature of Saturn's interior from the analysis of Saturn-driven waves in the rings. Here, we report the identification of six additional wave features, all in the inner C ring, from Cassini occultation measurements. Two of the waves are OLRs: Baillié feature #5 (B1 = W76.022 (i.e., r=76022 km)) with wavenumber m=-9, and Baillié #9 (B9 = W76.435) with m=-2. The first of these is presumably Saturn-driven, but of unknown origin; W76.435 fits very nicely in the pattern predicted by Marley (2014) for an m=l-2, q=2 internal oscillation. We also report the identification of a new class of Saturn-driven waves: B1 (W74.666), B3 (W74.936), B4 (W74.941), and B6 (W76.234) are all bending waves at Outer Vertical Resonances (OVR) with wavenumbers between m=-4 and m=-9

  18. Facts and Suggestions from a Brief History of the Galilean Moons and Space Weathering

    Science.gov (United States)

    Cooper, John

    2010-05-01

    energetic enough to change isotopic ratios in the affected surface materials. The sputtered materials partially escape either directly to the magnetosphere or indirectly through exospheric losses, so these additionally contribute at trace levels to the magnetospheric interconnections of surface composition for all the moons. In order to determine the intrinsic composition of the moons from EJSM surface and exospheric measurements, we must first peel back the surficial patina of space weathering products. Conversely, future measurements of the magnetospheric ion composition at high resolution in elemental and significant isotopic abundances, including as products of space weathering on the moon surfaces, can be projected back to the Io source for huge advancements of our knowledge on the origins of Io volcanism and more generally of the Jupiter system. These are some of the relevant facts for space weathering from 400 years of Jupiter system exploration, the main suggestion is that one the highest returns on international investments in the EJSM mission would be from advancement of capabilities for in-situ sample analysis in the magnetosphere and from moon surfaces to cover the full range of elements and key isotopes. Modest investments in appropriate technologies for ion and neutral gas measurements to this level would be insignificant in cost as compared to Earth sample return. This suggestion was submitted by Cooper et al. [4] to the ongoing decadal survey of planetary science and mission priorities in the United States. References: [1] Stebbins, J., Publ. Astron. Soc. Pacific 38 (225), 321-322, 1926; [2] Burke, B.F., and K. L. Franklin, J. Geophys. Res. 60, 213-217, 1955. [3] Morabito, L. A., et al., Science 204, 972, 1979; [4] Cooper, J. F., and 21 Co-authors, Space Weathering Impact on Solar System Surfaces and Mission Science, Community White Paper submitted to Planetary Science Decadal Survey, 2013--2022. National Research Council, Washington, D.C., Sept. 15, 2009.

  19. Solar Variability and Climate Change in the Last 2000 Years

    Science.gov (United States)

    Pang, K.; Yau, K.

    2002-12-01

    Studying past climatic data can help us better understand present natural variations and predict future trends. Identification of cycles can be useful to forecasting. However, various reconstructions of the climate of the last 1000 years have given only broad similarities, with large variances in time and space [Briffa JGR 106, 2929, 2001]. For example, during the Little Ice Age (ca. 1600-1800) severe winters were frequent in Europe and China, but not over Greenland [Sci. Amer., 2/1992, 21]. The differences in modeling results are partly due to uncertainties in the past radiative forcing [Mann, Eos 82 (46), 2001]. Another outstanding question is whether we are in a time similar to Medieval Warm Period. From the frequencies of sunspot and aurora sightings, abundance of carbon-14 in the rings of long-lived trees, and beryllium-10 in the annual layers of polar ice cores, we have reconstructed the recent history of a variable Sun. In the past 1800 years the Sun has gone through nine cycles of changes in brightness. While these long-term changes account for less than one percent of the total irradiance, there is a clear evidence that they affect the climate. During the Maunder Minimum (1645-1715) few sunspots were seen--about 1 in 10 yr from China or Europe--indicative of a weak Sun. Eddy [Science 192, 1189, 1976] used historical aurora, C-14 and climate data to confirm its reality, and link it to the Little Ice Age. Using new historical sunspot catalogues [Yau, Quart. J. Roy. Astron. Soc., 29, 175, 1988], we have identified or confirmed earlier solar minima at 200-300, 400-500, 580-820, 980-1070, 1280-1350, 1410-1590; and maxima at 1080-1280, 1350-1400, etc. All these features are coincident with respective minima or maxima in the frequency of aurora sightings from Europe or Asia. Both time series are in turn consistent with radioisotope data [Pang, Eos. 9/2002]. Carbon-14 and beryllium-10 are made by cosmic rays high in the atmosphere. When the Sun is active the solar

  20. Modelling detonation waves in condensed energetic materials: multiphase CJ conditions and multidimensional computations

    Science.gov (United States)

    Petitpas, F.; Saurel, Richard; Franquet, E.; Chinnayya, A.

    2009-10-01

    A hyperbolic multiphase flow model with a single pressure and a single velocity but several temperatures is proposed to deal with the detonation dynamics of condensed energetic materials. Temperature non-equilibrium effects are mandatory in order to deal with wave propagation (shocks, detonations) in heterogeneous mixtures. The model is obtained as the asymptotic limit of a total non-equilibrium multiphase flow model in the limit of stiff mechanical relaxation only (Kapila et al. in Phys Fluids 13:3002-3024, 2001). Special attention is given to mass transfer modelling, that is obtained on the basis of entropy production analysis in each phase and in the system (Saurel et al. in J Fluid Mech 607:313-350, 2008). With the help of the shock relations given in Saurel et al. (Shock Waves 16:209-232, 2007) the model is closed and provides a generalized ZND formulation for condensed energetic materials. In particular, generalized CJ conditions are obtained. They are based on a balance between the chemical reaction energy release and internal heat exchanges among phases. Moreover, the sound speed that appears at sonic surface corresponds to the one of Wood (A textbook of sound, G. Bell and Sons LTD, London, 1930) that presents a non-monotonic behaviour versus volume fraction. Therefore, non-conventional reaction zone structure is observed. When heat exchanges are absent, the conventional ZND model with conventional CJ conditions is recovered. When heat exchanges are involved interesting features are observed. The flow behaviour presents similarities with non ideal detonations (Wood and Kirkwood in J Chem Phys 22:1920-1924, 1950) and pathological detonations (Von Neuman in Theory of detonation waves, 1942; Guenoche et al. in AIAA Prog Astron Aeronaut 75: 387-407, 1981). It also present non-conventional behaviour with detonation velocity eventually greater than the CJ one. Multidimensional resolution of the corresponding model is then addressed. This poses serious

  1. Mal tiempo, tiempo maligno, tiempo de subversión ritual. La temposensitividad agrofestiva invernal

    Directory of Open Access Journals (Sweden)

    Del Campo Tejedor, Alberto

    2006-06-01

    Full Text Available In the light of a number of festive, ritual, poetico-musical and literary expresions, from Andalusia and elsewhere, the author discusses time as lived by agrarian cultures: a syncretic time, resulting from the superposition of civico-political, religious and peasant calendars; a cyclic time, given the effects of astronomico-meteorological time on nature and the subsequent cultural response on both the instrumental dimension (the work in the fields and the expresive dimension (the rituals and the festivals; and, finally, an ages-old bipolar time, experienced as the succession of two alternating seasons —wintertime and summertime—which also underlies a dichotomous agrofestive time-sensitiveness analyzed here under the following hypothesis: during the months of «good weather,» especially May and June, the rituals have a propitiatory and positively extolling sense; they mimetically dramatize the union between earth, vegetation, animals and humans by means of prototypes and archetypes that symbolically recreate the natural order of things. By contrast, the wintertime rituals and festivals—from 1st November till Carnival, and particularly around Christmas—all have in common a grotesque character and a sense of inverted order, symbolically signifying, with a logic at once serio-comic and ambiguous, the dark side of existence, while ritually conjuring up the fears of bad weather, of fateful and pernicious time, the time of cold nights, hunger and death.

    A la luz de algunas expresiones festivas, rituales, poético-musicales y literarias, de Andalucía y otros contextos, el artículo aborda el tiempo vivido por las culturas agroganaderas: un tiempo sincrético, como consecuencia de la superposición de los calendarios civil-político, religioso y campesino; un tiempo cíclico, fruto de la incidencia del tiempo astronómico-meteorológico en la naturaleza y la consiguiente respuesta cultural en el plano instrumental (los trabajos agr

  2. Analysis of astronomy knowledge of the students in the Federal Institute Sao Paulo

    Science.gov (United States)

    Moraes, A. C.; Voelzke, M. R.

    2014-08-01

    Este trabalho é parte integrante da pesquisa de mestrado acadêmico em ensino de ciências. Nele, busca-se apresentar os resultados da pesquisa realizada entre os 106 alunos do curso superior de tecnologia em automação industrial do Instituto Federal de Educação, Ciência e Tecnologia de São Paulo campus Cubatão, divididos em cinco turmas, duas no período matutino e três no período noturno. A análise dos resultados deste pré questionárioconstatou a falta de conhecimento básico dos discentes, sobre assuntos relacionados à astronomia, o que pode ser atribuído ao ineficiente processo de aprendizado pelo qual eles passaram tanto no ensino médio como no ensino fundamental, em escolas municipais, estaduais e particulares onde estudaram. No ensino de astronomia, têm-se diagnosticado constantemente diversas dificuldades conceituais tanto por parte de alunos como de professores de todas as áreas e níveis de ensino e poucos de fato a compreendem (ALBRECHT; VOELZKE, 2010). Demonstra-se as duas etapas concluídas do trabalho. A primeira etapa indica a análise dos conhecimentos prévios sobre conceitos astronômicos, através do questionário com 25 perguntas. A fim de corrigir as falhas constatadas, experimentalmente ministrou-se, externo ao conteúdo programático, um curso básico em astronomia, com diferentes estratégias de ensino, tais como, utilização de aulas expositivas dialogadas, recursos audiovisuais e palestras, para corrigir as dificuldades diagnosticadas. Essas estratégias de ensino se comprovaram adequadas às necessidades dos alunos e os conceitos foram finalmente compreendidos. Ao término do curso, completado o interstício de 120 dias, para caracterizar que houve a aprendizagem significativa, realizou-se uma nova pesquisa, quando, exatamente os mesmos 106 alunos responderam as mesmas 25 questões aplicadas na primeira etapa. Constata-se na segunda etapa, após análise, que em todas as questões, houve maior compreensão dos assuntos

  3. PLANET TOPERS: Planets, Tracing the Transfer, Origin, Preservation, and Evolution of their ReservoirS

    Science.gov (United States)

    Dehant, Veronique; Breuer, Doris; Claeys, Philippe; Debaille, Vinciane; De Keyser, Johan; Javaux, Emmanuelle; Goderis, Steven; Karatekin, Ozgur; Mattielli, Nadine; Noack, Lena; Spohn, Tilman; Carine Vandaele, Ann; Vanhaecke, Frank; Van Hoolst, Tim; Wilquet, Valerie

    2013-04-01

    The PLANET TOPERS (Planets, Tracing the Transfer, Origin, Preservation, and Evolution of their ReservoirS) group is an Inter-university attraction pole (IAP) addressing the question of habitability in our Solar System. Habitability is commonly understood as "the potential of an environment (past or present) to support life of any kind" (Steele et al., 2005, http://mepag.jpl.nasa.gov/reports/archive.html). Based on the only known example of Earth, the concept refers to whether environmental conditions are available that could eventually support life, even if life does not currently exist (Javaux and Dehant, 2010, Astron. Astrophys. Rev., 18, 383-416, DOI: 10.1007/s00159-010-0030-4). Life includes properties such as consuming nutrients and producing waste, the ability to reproduce and grow, pass on genetic information, evolve, and adapt to the varying conditions on a planet (Sagan, 1970, Encyclopedia Britannica, 22, 964-981). Terrestrial life requires liquid water. The stability of liquid water at the surface of a planet defines a habitable zone (HZ) around a star. In the Solar System, it stretches between Venus and Mars, but excludes these two planets. If the greenhouse effect is taken into account, the habitable zone may have included early Mars while the case for Venus is still debated. Important geodynamic processes affect the habitability conditions of a planet. As envisaged by the group, this IAP develops and closely integrates the geophysical, geological, and biological aspects of habitability with a particular focus on Earth neighboring planets, Mars and Venus. It works in an interdisciplinary approach to understand habitability and in close collaboration with another group, the Helmholtz Alliance "Life and Planet Evolution", which has similar objectives. The dynamic processes, e.g. internal dynamo, magnetic field, atmosphere, plate tectonics, mantle convection, volcanism, thermo-tectonic evolution, meteorite impacts, and erosion, modify the planetary surface

  4. The effect of dust charge fluctuations in the near-Enceladus plasma

    Science.gov (United States)

    Yaroshenko, Victoria; Luehr, Hermann

    charge fluctuations and resulting charge distribution in the parameter regime relevant for the Enceladus environment with a special emphasis on the limit of a dust-loaded plume. The stochastic charge fluctuations are studied in the light of the recent Cassini Plasma Spectrometer (CAPS) data on charged nanograins obtained during close Enceladus flybys [3]. It is our conclusion that in the dense plume the random charge fluctuations could indeed be in favor of observed dust characteristics, and they might be even responsible for the coexistence of negatively charged grain majority and a small amount of positively charged dust particles, as detected by CAPS. The obtained results might be also of importance for understanding the problem of dust transport in Saturn’s E ring. [1] M. Horányi, Annu. Rev. Astron. Astrophys., 34, 383, (1996). [2] V. V. Yaroshenko et al. J. Geophys. Res., DOI: 10.1002/2013JA019213, (2014) [3]T. W. Hill, et al., J. Geophys. Res., 117, A05209, (2012).

  5. Educação em Astronomia: contribuições de um curso de formação de professores em um espaço não formal de aprendizagem

    Directory of Open Access Journals (Sweden)

    Denise Fontanella

    2016-05-01

    Full Text Available Astronomy is a key area in Basic Education, and it provides an understanding of everyday phenomena. However, teachers and students have difficulties understanding the concepts in this area of knowledge. Thus the importance of this research is warranted to investigate the teacher training course on “Theoretical and Methodological Foundations for Teaching and Learning in Astronomy: Educator Training” offered by the “Polo Astronomical Casimiro Montenegro Filho”, located in Foz do Iguaçu, Brazil, and evaluate the perception of participating teachers in relation to the training performed. This is a qualitative work which used questionnaires, interviews, and records of the development of the course for data collection. Data were analyzed based on content analysis following the theory of Bardin (1977 and indicate that, with respect to the astronomy content, teachers have many difficulties because they lack quality initial or continuing education. Moreover, conceptual errors and misconceptions in issues related to astronomy were detected in researchers and course participants. The data indicate difficulties in teacher education regarding the area of Astronomy, but they present suggestions to alleviate these difficulties, such as the course for teacher training in Astronomy, which proved to be an ally of the teacher for working with contents, methodologies, and potentially usable resources in the classroom. A Astronomia é uma área fundamental na Educação Básica e proporciona a compreensão dos fenômenos cotidianos. Contudo, professores e alunos encontram dificuldades na compreensão dos conceitos dessa área do conhecimento. Desse modo, a importância dessa pesquisa se justifica ao investigar a formação de professores no curso “Fundamentos Teóricos e Metodológicos para o Ensino-Aprendizagem em Astronomia: Formação de Educadores” ofertado pelo “Polo Astronômico Casimiro Montenegro Filho”, localizado em Foz do Iguaçu, Brasil

  6. The DiskMass Survey. VI. Gas and stellar kinematics in spiral galaxies from PPak integral-field spectroscopy

    Science.gov (United States)

    Martinsson, Thomas P. K.; Verheijen, Marc A. W.; Westfall, Kyle B.; Bershady, Matthew A.; Schechtman-Rook, Andrew; Andersen, David R.; Swaters, Rob A.

    2013-09-01

    ROiii), with a zero point indicating that galaxy disks are submaximal. Moreover, weak but consistent correlations exist between σz,0/V2.2hROiii and global galaxy properties such that disks with a fainter central surface brightness in bluer and less luminous galaxies of later morphological types are kinematically colder with respect to their rotational velocities. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).Table 2 and Appendices are available in electronic form at http://www.aanda.org

  7. Photometric and spectroscopic evidence for a dense ring system around Centaur Chariklo

    Science.gov (United States)

    Duffard, R.; Pinilla-Alonso, N.; Ortiz, J. L.; Alvarez-Candal, A.; Sicardy, B.; Santos-Sanz, P.; Morales, N.; Colazo, C.; Fernández-Valenzuela, E.; Braga-Ribas, F.

    2014-08-01

    carbon, 30% of silicates and 10% of organics; no water ice was found on the surface. The ring, on the other hand, contains 20% of water ice, 40-70% of silicates, and 10-30% of tholins and small quantities of amorphous carbon. Partially based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile. DDT 291.C-5035(A). Based on observations carried out at the Complejo Astronómico El Leoncito, which is operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina and the National Universities of La Plata, Córdoba, and San Juan.

  8. Simplificando a luneta com lente de óculos

    Science.gov (United States)

    Canalle, J. B. G.; de Souza, A. C. F.

    2003-08-01

    A principal ferramenta de trabalho do astrônomo é o telescópio. O manuseio do mesmo é sempre motivo de enorme curiosidade por parte de alunos do ensino fundamental ou médio e até mesmo dos respectivos professores. Visando propiciar o acesso de alunos e professores ou interessados em geral a uma luneta de fácil construção, com materiais alternativos, de fácil localização no comércio, de baixo custo, resistente ao manuseio de alunos, simplificamos a montagem de uma luneta construída com lente de óculos, de 1 ou 2 graus positivos, e monóculo de fotografia, publicado por este autor no CCEF, vol.11(3), 212, 1994. Esta luneta, a qual permite ver as crateras lunares, apresentava como maior dificuldade de construção o tripé e o local de formação da imagem. Substituímos o tripé de madeira por uma simples garrafa PET de 2 litros cheia d'água. No lugar da ocular usamos a lente do monóculo de fotografia (ou visor de fotografia) encaixado dentro de uma bucha de redução curta, de 40 x 32 mm, e esta não mais dentro de uma luva (conexão hidráulica) de 40 mm de diâmetro, mas sim encostada no próprio tubo de PVC móvel (o qual permite o ajuste do foco) de 40 mm de diâmetro e presa a este por outro tubo de 40 mm de diâmetro e 10 cm de comprimento, serrado ao longo do seu comprimento. Com isto podemos ajustar a posição deste tubo de 10 cm também para que uma das suas extremidades coincida com o local de formação da imagem. Desta forma o observador saberá o local exato da formação da imagem, o que não era evidente na montagem anterior e causava uma dificuldade inicial até se descobrir a posição exata em que se deveria colocar o olho. Deste maneira, a montagem inicial que já era simples ficou ainda mais simples, mais barata e mais confortável para o uso. Um exemplar da mesma será exposto durante a XXIX Reunião Anual da Sociedade Astronômica Brasileira para inspeção e uso dos participantes.

  9. El boto y los geoglifos de Nasca: una contribución de la investigación estética en la arqueología

    Directory of Open Access Journals (Sweden)

    1974-01-01

    rito con la forma plástica del mismo y que se enlazan en un misterioso pero igualmente elocuente propósito. El arte como excedente de energías encuentra la posibilidad de llevar a cabo mediante este residuo de 'energía cultural', la forma que el mito exige para su significado. Esta manifestación no necesariamente ha de ser plástica puede ejercerse con otras formas de arte, bailes, cantos o lances deportivos, de competencia (al igual que el 'agón' griego que también pueden incluirse en este caso como expresión estética, en espacios rigurosamente señalados y consagrados en cumplimiento de esos ritos. Estos son los fundamentos de juicio crítico-estético que apoyan la tesis del autor La astrología (o religiosidad, puesto que hay armonía entre el astro solar y la existencia humana conjuga con el arte y desarrolla su actividad en los múltiples y complejos trazos-rectilíneos juntamente con oíros dibujos totémicos entrelazados y relacionados con estos trazos, algunos largos de kilómetros. Hace una memoria de su señalamiento y analiza el 'Informe Hawkins' como el más reciente y científico paso de investigación y que determina una fecha para la ejecución de estos trazos entre los años 390 a 500 de la era cristiana. Hawkins declara que estos trazos 'no parecen tener significado astronómico' por lo mismo cabe inclinarse hacia la hipótesis lúdicra del autor de este ensayo, como expresiones sociales en las que interviene un determinado sentido de juego, del deporte religioso. Entre los muchos glifos totémicos figura lo del cetáceo Boto (Orea gladiator que aparece ya en la cerámica del primer período cultural, el 'naturalista', que florece en los tiempos del sub-estilo 'nasca' de Lumbreras (100-300 d.C.. Comenta la posibilidad de errores en su trazo y señala el ejemplo como prueba de un rito que no es de una simple gratificación estética. Y deduce, de acuerdo con opiniones autorizadas, el desarrollo socio-político del 'genio' nasquense hasta su

  10. Interpretation of Titan's atmospheric composition measured by Cassini-Huygens

    Science.gov (United States)

    Tobie, G.; Gautier, D.; Hersant, F.; Lunine, J. I.

    2008-09-01

    released, but as its primordial abundance is small, it remains below the detection limit of the GCMS. The detection of the 40K decay daughter 40Ar is a strong indicator of past and recent internal activities, thus confirming the scenario proposed here. While most of the detected 40Ar comes from the silicate phase, which contains a significant fraction of potassium, we show that only a small fraction of the detected 36Ar can originate from the silicate phase. This strongly suggests that most of the primordial 36Ar has been brought by the ice phase, and that a fraction of argon, even if it is small, has been incorporated at low temperature in the planetesimals that built Titan in the form of clathrate hydrate. This favors the scenario where today's methane mainly originate from the solar nebula, was stored in the interior and later released; and thus was not chemically produced H2O and CO2 in the satellite interior. In situ measurements to be done by a future mission on Titan [4] will permit to test the different ideas present here. In particular, a precise determination of D/H and O16/O18 ratios in H2O, CO2 and CO will provide pertinent tests on the origin of different volatile species. IR spectroscopy and direct sampling of the surface materials will allow to determine the amount of carbon dioxide present in the crust. Detection of 38Ar, Kr and possibly Xe, and estimation of isotopic ratios will also give key informations on the origin and evolution of Titan's atmosphere and interior, in particular on the trapping mechanismes of volatile in Saturn's environnement and on the differentiation processes of Titan's interior. References [1] Niemann, H. B., and 17 colleagues 2005. Nature 438, 779-784. [2] Hersant, F., Gautier, D., Tobie, G., Lunine, J. I. 2008. Planet Space Sci., in press. [3] Tobie, G., Lunine, J. I., Sotin, C. 2006. Nature, 440, 61-64. [4] Coustenis A. and the TANDEM consortium, 2008. Experimental Astron., in press.

  11. Book Reviews

    Directory of Open Access Journals (Sweden)

    Peter Metcalf

    1990-10-01

    age in motion; Popular radicalism in Java, 1912-1926, Ithaca/London: Cornell University Press, 1990. xxiv + 365 pp. - Rob de Ridder, Willem F.H. Adelaar, Het boek van Huarochirí. Mythen en riten van het Oude Peru, Amsterdam: Meulenhoff, 1988, 150 pp., - Marie-Odette Scalliet, Peter Carey, A.A.J. Payen: Journal de mon voyage à Jogja Karta en 1825. The outbreak of the Java War (1825-30 as seen by a painter, Cahier d’Archipel 17, Paris 1988. XIV + 183 pp., 17 ill., 3 maps. - Matthew Schoffeleers, Marion Melk-Koch, Auf der Suche nach der menschlichen Gesellschaft: Richard Thurnwald, Berlin: Dietrich Reimer, 1989. 352 pp., maps, photographs and Thurnwald bibliography. - Matthew Schoffeleers, Peter Metcalf, Where are you / Spirits? Style and theme in Berawan prayer, Washington and London: Smithsonian Institution Press, 1989, 345 pp. - J.W. Schoorl, J.F.L.M. Cornelissen, Pater en Papoea; Ontmoeting van de Missionarissen van het Heileg Hart met de cultuur der Papoea’s van Nederlands Zuid-Nieuw-Guinea (1905-1963, Kampen: Kok, 1988, XIV + 256 pp. - Alex van Stipriaan, Jo Derkx, Suriname; A bibliography, 1980-1989, Leiden: KITLV (Royal Institute of Linguistics and Anthropology, Department of Caribbean studies, 1990, 297 pp., Irene Rolfes (eds. - A.A. Trouwborst, Th. Schweizer (Hg, Netzwerkanalyse; Ethnologische perspektiven, Berlin: Dietrich Reimerverlag, 1989, VIII, 229 pp. - Hans Vermeulen, Brian Juan O’Neill, Social inequality in a Portugese hamlet; Land, late marriage and bastardy, 1870-1978, Cambridge: Cambridge University Press. 431 pp. 1987. - C.W. Watson, Hendrick M.J. Maier, In the center of authority. The Malay Hikayat Merong Mahawangsa, Ithaca: Southeast Asia program, Studies on Southeast Asia , 1988. 210 pp. - Neil Lancelot Whitehead, Edmundo Magaña, Orión y la mujer Pléyades. Simbolismo astronómico de los indios kaliña de Surinam, Dordrecht/Providence: Foris, 1988. [CEDLA Latin American studies series 44.] 373 pp. - J.J. de Wolf, Meyer Fortes, Religion

  12. Poluição atmosférica e atendimentos por pneumonia e gripe em São Paulo, Brasil Air pollution and emergency room visits due to pneumonia and influenza in São Paulo, Brazil

    Directory of Open Access Journals (Sweden)

    Lourdes Conceição Martins

    2002-02-01

    Full Text Available OBJETIVO: Investigar os efeitos causados pela poluição atmosférica na morbidade por pneumonia e por gripe em idosos entre 1996 e 1998. MÉTODOS: Foram obtidos dados diários de atendimentos por pneumonia e gripe para idosos em pronto-socorro médico de um hospital-escola de referência no Município de São Paulo, SP, Brasil. Os níveis diários de CO, O3, SO2, NO2 e PM10 foram obtidos na Companhia de Tecnologia de Saneamento Ambiental, e os dados diários de temperatura e umidade relativa do ar foram obtidos no Instituto Astronômico e Geofísico da USP. Para verificar a relação existente entre pneumonia e gripe e poluição atmosférica, utilizou-se o modelo aditivo generalizado de regressão de Poisson, tendo como variável dependente o número diário de atendimentos por pneumonia e gripe e como variáveis independentes as concentrações médias diárias dos poluentes atmosféricos. A análise foi ajustada para sazonalidade de longa duração (número de dias transcorridos, sazonalidade de curta duração (dias da semana, temperatura mínima, umidade média, períodos de rodízio e os atendimentos por doenças não-respiratórias em idosos. RESULTADOS: O3 e SO2 estão diretamente associados à pneumonia e à gripe, independentemente das variáveis de controle. Porém, na análise conjunta, eles perdem sua significância estatística. Pôde-se observar que um aumento interquartil (25%-75% para o O3 (38,80 mig/m³ e SO2 (15,05 mig/m³ levaram a um acréscimo de 8,07% e 14,51%, respectivamente, no número de atendimentos por pneumonia e gripe em idosos. CONCLUSÕES: Os resultados sugerem que a poluição atmosférica promove efeitos adversos para a saúde de idosos.OBJECTIVE: A time series was developed to investigate the effect of air pollution levels on morbidity due to respiratory diseases such as pneumonia and influenza among elderly people from 1996 to 1998. METHODS: Daily data on emergency room visits was collected at the university

  13. Mixed-Methods Study that Examines Nine Science Teachers' Perceptions of Slooh Robotic Telescope for Teaching Astronomy. (Breton Title: Métodos Mistos de Estudo que Examinam a Percepção de Nove Professores de Ciências sobre o Telescópio Robótico Slooh Para Ensino de Astronomia.) Métodos Mixtos de Estudio que Examinan la Percepcion de Nueve Profesores de Ciencias sobre EL Telescopio Robótico Slooh Para la Enseñanza de la Astronomía

    Science.gov (United States)

    Gershun, Daniel C.; Slater, Timothy F.; Berryhill, Katie J.

    2014-07-01

    ção em sala de aula", "Impacto no Instrutor" e "Questões logísticas". A análise desses temas sugere que Slooh pode proporcionar um ambiente de aprendizagem interativo e social com capacidade de incorporar temas interdisciplinares. Aunque estudios previos muostraron que los telescopios robóticos tienen el potencial de mejorar el aprendizaje del estudiante, hay relativamente poca investigación centrada en las percepciones de lós profesores respecto de esta tecnología. Este estudio investiga: "¿cuál es el mérito académico de la utilización de telescopios robóticos SLOOH para enseñar astronomía según la percepción de los profesores de ciências?" Nuestra muestra está formada por nueve profesores de ciencias de estudiantes entre 13 a 18 años pre-y post-tests, entrevistas, y. encuestas se recogieron durante dos semanas de un curso on-line de verano sobre los telescopios robóticos. Si bien lós tests antes y después de las pruebas no revelaron un aumento estadísticamente significativo en el conocimiento de contenido astronómico, el análisis de lós datos cualitativos reveló cinco temas que describen los aspectos más importantes de la utilización de SLOOH de acuerdo con los participantes:. "Imágenes", "Interface", "aplicación en el aula", "Impacto en el Instructor" y "problemas logísticos" . El análisis de estos temas sugiere que SLOOH puede proporcionar un ambiente de aprendizaje interactivo y social, con capacidad para incorporar temas transversales.

  14. Oxygen Isotope Anomalies in Orgueil Corundum: Confirmation of Presolar Origin

    Science.gov (United States)

    Huss, G. R.; Hutcheon, I. D.; Fahey, A. J.; Wasserburg, G. J.

    1993-07-01

    mean value of delta^17O = -45.1 +- 2.1 per mil and delta^18O = -41.2 +- 2.2 per mil, very similar to the composition of Allende CAI spinel [8]. The Orgueil spinel and hibonite are slightly less ^16O-rich with delta^18O values between -18 per mil and -42 per mil. One Orgueil spinel and four corundums have normal O-isotope compositions with delta^17O ~ delta^18O ~ 0. The only other refractory oxide grains with similar composition are a group of Cr-rich Murchison spinel [9]. Two Orgueil corundums are enriched in the heavier O-isotopes and have compositions falling along the terrestrial fractionation line (delta^17O ~ 42 per mil, delta^18O ~ 75 per mil). This is the heaviest oxygen isotopic composition reported in meteoritic materials. If this composition is derived from isotopically normal oxygen by mass-dependent fractionation, the magnitude of fractionation is similar to that measured in the Allende FUN inclusion HAL [10]. References: [1] Huss G. R. et al. (1992) LPS XXIII, 563. [2] Zinner E. K. et al. (1991) Nature, 349, 51. [3] Nittler L. R. et al. (1993) LPS XXIV, 1087. [4] Lambert D. L. (1988) In Evolution of Peculiar Red Giant Stars, 101. [5] Forestini M. et al. (1991) Astron. Astrophys., 252, 597. [6] Wasserburg G. J. et al. (1993) LPS XXIV, 1487. [7] Virag S. A. et al. (1991) GCA, 55, 2045. [8] Clayton R. N. et al. (1977) EPSL, 34, 209. [9] Grossman L. et al. (1988) LPS XIX, 435-436. [10] Lee T. et al. (1980) GRL, 7, 498- 496. Division Contribution 5273(815); NASA NAGW-3297. Fig. 1, which appears here in the hard copy, shows oxygen isotopic composition of refractory oxide grains from Orgueil and Allende. The insert is an expanded view of the region inside the open box, near delta^17O ~ delta^18O ~ 0. The solid lines in the insert represent the terrestrial fractionation line (slope = 1/2) and the ^16O-mixing line (slope = 1). Ratios are shown as the per mil deviation from SMOW; errors are +-2 sigma(sub)mean.

  15. Brennand: resonancia y universalidad de las formas Brennand: resonance and the univesality of the forms

    Directory of Open Access Journals (Sweden)

    G. CECILIA TORO

    2001-03-01

    Full Text Available Este trabajo propone la búsqueda y exposición de patrones de formas, tanto de algunas obras producidas por la naturaleza como de algunas de las obras producidas por la mano del hombre, quien como un microcosmos, que forma parte de la naturaleza recrea el macrocosmos. En una cultura en que el hombre ha perdido contacto con la naturaleza, con sus semejantes y con sus orígenes, otro objetivo de este trabajo es re emparentar al hombre con la naturaleza de la que forma parte. Se pretende mostrar al hombre, como un fractal del Universo, que es capaz de recrear, independientemente del tiempo, del espacio y de la escala de magnitudes, las mismas formas que crea el Universo, con la fuerza de la belleza en toda su pureza y en todo lo terrible con que a veces se nos presenta su aspecto. La belleza, así como la religión o como la pureza, tiene un poder redentor y el hombre anhela los paraísos perdidos. Cuando se amplia nuestra capacidad para percibir la belleza ya estamos en camino cierto, ya estamos en un camino que nos cambia desde un estado de conciencia a otro, ya estamos en un camino de regreso a la unidad. En el presente estudio se exponen algunas formas durante la diferenciación de un platelminto, Mesocestoides corti, obtenidas mediante microscopía de barrido y se exponen algunas obras de un hombre, Francisco Brennand, ganador del premio Gabriela Mistral 1993, el mayor premio dado en artes plásticas en América. Brennand, como un holograma, con un único referencial: el Universo ha recreado un Universo biológico y de increíble belleza desde su interior. En este trabajo, se pretende además exponer como, a través de la historia de nuestra cultura, el hombre justificó el anhelo y la certeza de universalidad, generando explicaciones filosóficas, psicológicas, biológicas, físicas, matemáticas, astronómicas y artísticasThis work proposes for the search and exposition of patterns of forms as they appear in nature as well as those

  16. Nuclear planetology: understanding planetary mantle and crust formation in the light of nuclear and particle physics

    Science.gov (United States)

    Roller, Goetz

    2017-04-01

    conceptual model constraining the evolution of a rocky planet like Earth or Mercury from a stellar precursor of the oldest population to a Fe-C BLD, shifting through different spectral classes in a HR diagram after massive decompression and tremendous energy losses. In the light of WD/BLD cosmochronology [1], solar system bodies like Earth, Mercury and Moon are regarded as captured interlopers from the Galactic bulge, Earth and Moon possibly representing remnants of an old binary system. Such a preliminary scenario is supported by similar ages obtained from WD's for the Galactic halo [1] and, independently, by means of 187Re-232Th-238U nuclear geochronometry [3, 4], together with recent observations extremely metal-poor stars from the cosmic dawn in the bulge of the Milky Way [8]. This might be further elucidated in the near future by Th/U cosmochronometry based upon a nuclear production ratio Th/U = 0.96 [9] and additionally by means of a newly developed nucleogeochronometric age dating method for stellar spectroscopy [9-11]. The model shall stimulate geochemical data interpretation from a different perspective, to constrain the evolution and differentiation of planetary or lunar crusts and mantles in general. [1] Fontaine et al. (2001), Public. Astron. Soc. of the Pacific 113, 409-435. [2] Roller (2015), Abstract T34B-0407, AGU Spring Meeting 2015. [3] Roller (2016), Goldschmidt Conf. Abstr. 26, 2642. [4] Roller (2015), Goldschmidt Conf. Abstr. 25, 2672. [5] Roller (2015), Geophys. Res. Abstr. 18, EGU2016-33. [6] Arevalo et al. (2010), Chem. Geol. 271, 70-85. [7] Roller (2015), Geophys. Res. Abstr. 17, EGU2015-2399. [8] Howes et al. (2015), Nature 527, 484-487. [9] Roller (2016), JPS Conf. Proc., Nuclei in the Cosmos (NIC XIV), Niigata, Japan, subm. (NICXIV-001); NICXIV Abstr. #1570244284. [10] Roller (2016), JPS Conf. Proc., Nuclei in the Cosmos (NIC XIV), Niigata, Japan, subm. (NICXIV-002); NICXIV Abstr. #1570244285. [11] Roller (2016), JPS Conf. Proc., Nuclei in the

  17. Chemical composition of the semi-volatile grains of comet 67P/Churyumov-Gerasimenko

    Science.gov (United States)

    Wurz, Peter; Altwegg, Kathrin; Balsiger, Hans; Berthelier, Jean-Jacques; Bieler, André; Calmonte, Ursina; De Keyser, Johan; Fiethe, Björn; Fuselier, Stefan; Gasc, Sébastien; Gombosi, Tamas; Jäckel, Annette; Korth, Axel; Le Roy, Lena; Mall, Urs; Rème, Henri; Rubin, Martin; Tzou, Chia-Yu

    2017-04-01

    Neutral Analysis, Space Science Review 128 (2007), 745-801. K.-H Glassmeier, H. Boehnhardt, D. Koschny, E. Kührt, and I. Richter, The Rosetta Mission: Flying To-wards the Origin of the Solar System, Space Science Reviews 128 (2007), 1-21. S. Scherer, K. Altwegg, H. Balsiger, J. Fischer, A. Jäckel, A. Korth, M. Mildner, D. Piazza, H. Rème, and P. Wurz, A novel principle for an ion mirror design in time-of-flight mass spectrometry, Int. Jou. Mass Spectr. 251 (2006) 73-81. P. Wurz, M. Rubin, K. Altwegg, H. Balsiger, S. Gasc, A. Galli, A. Jäckel, L. Le Roy, U. Calmonte, C. Tzou, U.A. Mall, B. Fiethe, J. De Keyser, J.J. Berthelier, H. Rème, A. Bieler, V. Tenishev, T.I. Gombosi, and S.A. Fuselier, Solar Wind Sputtering of Dust on the Surface of 67P/Churyumov-Gerasimenko, Astron. Astrophys. 583, A22 (2015) 1-9, DOI: 10.1051/0004-6361/201525980.

  18. A Look into the Hellish Cradles of Suns and Solar Systems

    Science.gov (United States)

    2009-09-01

    Rose, T.L. Bourke, R.A. Gutermuth and S.J. Wolk (Harvard-Smithsonian Center for Astrophysics, Cambridge, USA), S.T. Megeath (Department of Physics and Astronomy, The University of Toledo, USA), J. Alves (Centro Astronómico Hispano Alemán, Almeria, Spain), and D. Nürnberger (ESO). ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe and the world's most productive astronomical observatory. It is supported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in Chile: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope, the world's most advanced visible-light astronomical observatory. ESO is the European partner of a revolutionary astronomical telescope ALMA, the largest astronomical project in existence. ESO is currently planning a 42-metre European Extremely Large optical/near-infrared Telescope, the E-ELT, which will become "the world's biggest eye on the sky".

  19. A proposed contents astronomy for basic education

    Science.gov (United States)

    Albrecht, E.; Voelzke, M. R.

    2014-08-01

    A Astronomia é um tema que sempre exerceu fascínio sobre as pessoas de um modo geral. Conhecer e estudar o que há nos “céus”, além de nossos olhos, continua sendo instigador e de grande interesse. Baseado nestas justificativas desenvolveu-se uma pesquisa de Doutorado, na qual, o objetivo principal foi investigar sobre a presença dos conteúdos de Astronomia nas Propostas Curriculares da região Sul do Brasil, a saber, os estados de Paraná, Rio Grande do Sul e Santa Catarina e, posterior comparação com os Parâmetros Curriculares Nacionais (PCN) que trazem propostas de conteúdos para toda a Educação Básica brasileira. Tal investigação pautou-se na abordagem de caráter qualitativo e utilizouse para tal da Análise de Conteúdos (Bardin, 2011), que possibilitou a construção de quatro categorias, nas quais os conteúdos astronômicos foram agrupados: Terra, Sistema Solar, Via Láctea e Universo. Após a leitura, coleta de dados, construção de categorias, observou-se a dicotomia na apresentação destes conteúdos. As propostas curriculares analisadas foram as de Geografia, Ciências e Física dos estados do Paraná (2008), Rio Grande do Sul (2009) e de Santa Catarina (1998), responsáveis pelo trabalho com Astronomia nestes estados. No Ensino Fundamental, a proposta curricular do estado do Paraná apresenta conteúdos ligados à Astronomia desde o sexto ano até o nono ano, como conteúdo do primeiro bimestre, o que também é apresentado na proposta curricular do estado do Rio Grande do Sul, porém, este, não divide os conteúdos por bimestre e nem por ano, mas por ciclos, sexto e sétimo anos como primeiro ciclo e oitavo e nono anos como segundo ciclo, deixando livre para o professor estruturar sua sequência de conteúdos. A proposta curricular de Santa Catarina não apresenta estes conteúdos de maneira explícita, não divide dos conteúdos nem por ano, nem por série, traz uma sequência de conteúdos para serem trabalhados ao longo dos

  20. Aromatic and aliphatic organic materials on Iapetus: Analysis of Cassini VIMS data

    Science.gov (United States)

    Cruikshank, Dale P.; Dalle Ore, Cristina M.; Clark, Roger N.; Pendleton, Yvonne J.

    2014-05-01

    , D.P., Clark, R.N. [2012], op. cit.) and Phoebe (Dalle Ore, C.M., Cruikshank, D.P., Clark, R.N. [2012], op. cit.). Our Gaussian decomposition of the organic band region suggests the presence of molecular bands in addition to those noted above, specifically bands attributable to cycloalkanes, olefinic compounds, CH3OH, and N-substituted PAHs, as well as possible Hn-PAHs (PAHs with excess peripheral H atoms). In a minimalist interpretation of the Gaussian band fitting, we find the ratio of aromatic CH to aliphatic CH2 + CH3 functional groups for both the leading and trailing hemispheres of Iapetus is ∼10, with no clear difference between them. In the aliphatic component of the surface material, the ratio CH2/CH3 is 4.0 on the leading hemisphere and 3.0 on the trailing; both values are higher than those found in interstellar dust and other Solar System materials and the difference between the two hemispheres may be statistically significant. The superficial layer of low-albedo material on Iapetus originated in the interior of Phoebe and is being transported to and deposited on Iapetus (and Hyperion) in the current epoch via the Phoebe dust ring (Tosi, F., Turrini, D., Coradini, A., Filacchione, G., and the VIMS Team [2010]. Mon. Not. R. Astron. Soc. 403, 1113-1130; Tamayo, D., Burns, J.A., Hamilton, D.P., Hedman, M.M. [2011]. Icarus 215, 260-278). The PAHs on Iapetus exist in a H2O-rich environment, and consequently are subject to UV destruction by hydrogenation on short time-scales. The occurrence of this material is therefore consistent with the assertion that the deposition of the PAH-bearing dust is occurring at the present time. If the organic inventory we observe represents the interior composition of Phoebe, we may be sampling the original material from a region of the solar nebula beyond Neptune where Phoebe formed prior to its capture by Saturn (Johnson, T.V., Lunine, J.I. [2005]. Nature 435, 69-71).

  1. On the roto-translatory internal motions of a three layer non-isobarycentric Earth model: a Lagrangian system approach

    Science.gov (United States)

    Escapa, Alberto; Fukushima, Toshio

    2010-05-01

    simply a kinematical correction on the degenerate mode of a non-rotating model. Namely, the relative errors in the periods of the equatorial modes are reduced from 11.69% to 3.79% and from -6.04% to -1.91%, respectively. Acknowledgement.- AE's contribution was carried out thanks to a sabbatical leave from the University of Alicante at the National Astronomical Observatory of Japan (NAOJ), supported by the Spanish Ministerio de Educación, project PR2009-0379, within the Programa Nacional de Movilidad de Recursos Humanos I-D+i 2008-2011. The generous hospitality of the NAOJ staff is gratefully acknowledged. References Busse, F.H., J. Geophys. Res. 79, 753, 1974 Getino, J. and Ferrándiz, J. M., Mon. Not. R. Astron. Soc. 322, 785, 2001 Moritz, H., Bull. Géod., 56, 364, 1982 Rieutord, M., Phys. Earth Planet. Int., 131, 269, 2002

  2. Hot Spot Cosmic Accelerators

    Science.gov (United States)

    2002-11-01

    cosmic objects. Notes [1]: The new results are described in a research paper, "Particle Accelerators in the Hot Spots of Radio Galaxy 3C 445, Imaged with the VLT" by M. Almudena Prieto (ESO, Garching, Germany), Gianfranco Brunetti (Istituto de Radioastronomia del CNR, Bologna, Italy) and Karl-Heinz Mack (Istituto de Radioastronomia del CNR, Bologna, Italy; ASTRON/NFRA, Dwingeloo, The Netherlands; Radioastronomisches Institut der Universität Bonn, Germany), that recently appeared in the research journal Science (Vol. 298, pp. 193-195). [2]: When electrons - which are electrically charged - move through a magnetic field, they spiral along the lines of force. Electrons of high energy spiral very rapidly, at speeds near the speed of light. Under such conditions, the electrons emit highly polarized electromagnetic radiation. The intensity of this radiation is related to the strength of the magnetic field and the number and energy distribution of the electrons caught in this field. Many cosmic radio sources have been found to emit synchrotron radiation - one of the best examples is the famous Crab Nebula, depicted in ESO PR Photo 40f/99. ESO PR Photo 26/02 may be reproduced, if credit is given to the European Southern Observatory (ESO) and the US National Radio Astronomy Observatory (NRAO).

  3. A New Clue in the Mystery of Fast Radio Bursts

    Science.gov (United States)

    Kohler, Susanna

    2017-06-01

    The origin of the mysterious fast radio bursts has eluded us for more than a decade. With the help of a particularly cooperative burst, however, scientists may finally be homing in on the answer to this puzzle.A Burst RepeatsThe host of FRB 121102 is placed in context in this Gemini image. [Gemini Observatory/AURA/NSF/NRC]More than 20 fast radio bursts rare and highly energetic millisecond-duration radio pulses have been observed since the first was discovered in 2007. FRB 121102, however, is unique in its behavior: its the only one of these bursts to repeat. The many flashes observed from FRB 121102 allowed us for the first time to follow up on the burst and hunt for its location.Earlier this year, this work led to the announcement that FRB 121102s host galaxy has been identified: a dwarf galaxy located at a redshift of z = 0.193 (roughly 3 billion light-years away). Now a team of scientists led by Cees Bassa (ASTRON, the Netherlands Institute for Radio Astronomy) has performed additional follow-up to learn more about this host and what might be causing the mysterious flashes.Hubble observation of the host galaxy. The object at the bottom right is a reference star. The blue ellipse marks the extended diffuse emission of the galaxy, the red circle marks the centroid of the star-forming knot, and the white cross denotes the location of FRB 121102 ad the associated persistent radio source. [Adapted from Bassa et al. 2017]Host ObservationsBassa and collaborators used the Hubble Space Telescope, the Spitzer Space Telecsope, and the Gemini North telecsope in Hawaii to obtain optical, near-infrared, and mid-infrared observations of FRB 121102s host galaxy.The authors determined that the galaxy is a dim, irregular, low-metallicity dwarf galaxy. Its resolved, revealing a bright star-forming region roughly 4,000 light-years across in the galaxys outskirts. Intriguingly, the persistent radio source associated with FRB 121102 falls directly within that star-forming knot

  4. ASPECTOS RELEVANTES DA APROXIMAÇÃO ENTRE BRASIL E CHINA: UMA ABORDAGEM ANALÍTICA [doi: 10.5329/RECADM.20050401009

    Directory of Open Access Journals (Sweden)

    Silvio Aparecido Crepaldi

    2005-05-01

    Full Text Available Normal 0 21 false false false PT-BR X-NONE X-NONE MicrosoftInternetExplorer4 RESUMO Nos últimos anos, cresceu notavelmente o interesse mútuo entre o Brasil e a China. Na década de 1990 ambos os países se esforçaram para promover a multi-polarização do poder mundial e fortalecer a cooperação entre países em desenvolvimento. Brasil e China trabalham com vistas à consolidação de uma parceria estratégica, o que tem impulsionado as relações bilaterais; mas há ainda desafios a serem superados. Com esta realidade surge uma lacuna na bibliografia sobre os aspectos relevantes da aproximação Brasil e China. Assim, a carência de bibliografias voltadas ao assunto que incluam o estudo desta aproximação e seus reflexos, motiva à pesquisa visando sanar essas deficiências. Pretende-se analisar as relações comerciais sino-brasileiras de 1984 a 2002 e explorar o significado do conceito de parceria estratégica no relacionamento dos dois países. Antes disso, contudo, são indispensáveis algumas ponderações extraídas da sua análise global, permitindo a melhor reflexão e apontamento de conclusões sobre as relevantes matérias tratadas na referida aproximação Brasil e China. Em conseqüência do cenário exposto, a problemática pode ser sintetizada na seguinte questão: "como Brasil e China deveriam interagir entre si para obter uma inserção mutuamente vantajosa no mundo globalizado?". As informações referentes ao tema aproximação entre Brasil e China foram obtidas mediante pesquisa bibliográfica. O volume das transações comerciais entre Brasil e China vem evoluindo rapidamente e a China tornou-se recentemente o maior parceiro comercial do Brasil na Ásia. Há ainda enormes potencialidades comerciais a serem exploradas. Ao mesmo tempo, a economia chinesa consegue gerar empregos urbanos em escala astronômica. Somente nos primeiros 9 (nove meses deste ano, foram criados cerca de 8 milhões de postos de trabalho nas cidades

  5. Editorial

    Science.gov (United States)

    Dimitrijevic, M. S.; Popovic, L. C.

    The present issue of SERBIAN ASTRONOMICAL JOURNAL is the last one edited by the two of us. We resigned not because we were tired of our service to the astronomical community but due to the old tradition of the Belgrade Astronomical Observatory that its Director is automatically the Editor-in-Chief of its publications. We therefore gladly give the opportunity to the new Director, in charge since July 1st. 2002, to organize the publishing activity according to his conceptions. One of us (M.S.D.) was appointed Editor on January 1st. 1984 (from No. 135), becoming the Editor-in-Chief in 1987 (from No. 137). The other one (L.C.P.) is the Editor since 1994 (from No. 150). During this period the Bulletin de l'Observatoire Astronomique de Belgrade merged with the Publications of the Department of Astronomy, changing its name into Bulletin Astronomique de Belgrade from No. 145 in 1992, to finally become Serbian Astronomical Journal in 1998, from No. 157. Accordingly, of a "Bulletin" we made a "Journal". For example, in the period 1971-1984 (Nos. 125-134) in Bull. Obs. Astron. Belgrade, practically only the associates of the Belgade Observatory published their papers, save for a few individuals from the Belgrade University. We found within this period the name of one sole foreign astronomer - from the USSR - namely V. A. Fomin, among the authors. In the period 1985-2002 in the Serbian Astronomical Journal published their communications not only astronomers from Yugoslavia but also from Belgium, China, France, Italy, Moldova, Romania, Russia, Spain, Ukraine, USA. Our authors from outside of Yugoslavia are: J. P. Anosova C. Beuyninx Cristina Blaga Paul A. Blaga Veronique Bommier N. M. Bronnikov Alberto Celino Pierre Cugnon D. R. Davis Henry Debehogne Veronique Dehant P. Farinella Alex Gaina R. I. Gumerov R. S. Izmailov V. B. Kapkov F. F. Khalikhevich S. A. Kilioner Tatiana R. Kirian N. G. Litkevich Evencio G. Mediavilla O. Mihai Andrea Milani Vasile Mioc Jose A. Munoz Viktor V

  6. Ideas de Vida y Muerte en Culturas Orientales

    Directory of Open Access Journals (Sweden)

    Adolfo de Francisco Zea

    1994-12-01

    Full Text Available

    Señor Presidente: Es muy placentero para mí en la tarde de hoy entregar a la Academia por su digno conducto, el retrato del Dr. Luis Zea Uribe, mi abuelo, quien fuera miembro de la Corporación por largo tiempo y presidiera sus destinos de 1928 a 1930.y es especialmente significativo para mí por ser usted, mi compañero de estudios y amigo de siempre, quien ocupa hoy con lujo y distinción la Presidencia de la Academia.

    Este retrato es copia del que fuera pintado por el célebre miniaturista y retratista bogotano Luis Felipe Uzcátegui hace varias décadas y hace justicia a las inmensas calidades de su espíritu: la frente amplia que traduce una inteligencia prodigiosamente lúcida, rápida y penetrante hasta lo maravilloso, como lo señalara Armando Solano en el prólogo del libro que recogió sus Producciones Escogidas.

    Las líneas delgadas de su boca y el mentón recio del estudioso que además de adquirir amplios conocimientos médicos, incursionó con su microscopio monocular en el mundo de lo infinitamente pequeño y apreció con su telescopio el mundo de lo infinitamente grande, lo que lo condujo a ser miembro de la Sociedad Astronómica de Francia presidida en ese entonces por su amigo cercano Camilo Flammarion. Quizás fue el estudio de las maravillas del universo lo que lo llevó un paso adelante a investigar en el campo de los fenómenos espiritualistas que hoy caen dentro de la órbita de la psicología y la para psicología, para lo cual estaba admirablemente dotado. Allí adquirió la certeza absoluta de la existencia del más allá y de un Dios inefable pleno de bondad y ordenó su vida entera a adquirir el Conocimiento, a impregnar todos sus actos con un alto sentido de la ética y a buscar el perfeccionamiento personal en la existencia terrena, que en su sentir, habría de permitirle en sucesivas encarnaciones acercarse cada vez más a la perfección.

    Sus experiencias en el campo espiritualista y sus

  7. Radio Telescopes Will Add to Cassini-Huygens Discoveries

    Science.gov (United States)

    2004-12-01

    telescopes in Parkes, Mopra, and Ceduna, Australia; Hobart, Tasmania; Urumqi and Shanghai, China; and Kashima, Japan. The positional measurements are a project led by JIVE and involving ESA, the Netherlands Foundation for Research in Astronomy, the University of Bonn, Helsinki University of Technology, JPL, the Australia Telescope National Facility, the National Astronomical Observatories of China, the Shanghai Astronomical Observatory, and the National Institute for Communication Technologies in Kashima, Japan. The Joint Institute for VLBI in Europe is funded by the national research councils, national facilities and institutes of The Netherlands (NWO and ASTRON), the United Kingdom (PPARC), Italy (CNR), Sweden (Onsala Space Observatory, National Facility), Spain (IGN) and Germany (MPIfR). The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.

  8. Astronomers Make First Images With Space Radio Telescope

    Science.gov (United States)

    1997-07-01

    part of the VLBA instrument, was modified over the past four years to allow it to incorporate data from the satellite. Correlation of the observational data was completed successfully on June 12, after the exact timing of the satellite recording was established. Further computer processing produced an image of PKS 1519-273 -- the first image ever produced using a radio telescope in space. For Jim Ulvestad, the NRAO astronomer who made the first image, the success ended a long quest for this new capability. Ulvestad was involved in an experiment more than a decade ago in which a NASA communications satellite, TDRSS, was used to test the idea of doing radio astronomical imaging by combining data from space and ground radio telescopes. That experiment showed that an orbiting antenna could, in fact, work in conjunction with ground-based radio observatories, and paved the way for HALCA and a planned Russian radio astronomy satellite called RadioAstron. "This first image is an important technical milestone, and demonstrates the feasibility of a much more advanced mission, ARISE, currently being considered by NASA," Ulvestad said. The first image showed no structure in the object, even at the extremely fine level of detail achievable with HALCA; it is what astronomers call a "point source." This object also appears as a point source in all-ground-based observations. In addition, the 1986 TDRSS experiment observed the object, and, while this experiment did not produce an image, it indicated that PKS 1519-273 should be a point source. "This simple point image may not appear very impressive, but its beauty to us is that it shows our entire, complex system is functioning correctly. The system includes not only the orbiting and ground-based antennas, but also the orbit determination, tracking stations, the correlator, and the image-processing software," said Jonathan Romney, the NRAO astronomer who led the development of the VLBA correlator, and its enhancement to process data

  9. S-N secular ocean tide: explanation of observably coastal velocities of increase of a global mean sea level and mean sea levels in northern and southern hemispheres and prediction of erroneous altimetry velocities

    Science.gov (United States)

    Barkin, Yury

    2010-05-01

    levels have been obtained at set of simplifying assumptions concerning of a direction of drift of the centre of mass of the Earth and character of redistribution of atmospheric and oceanic masses and, naturally, in future will be specified. The work was accepted by grants of RFBR: N 07-05-00939. References [1] Barkin Yu.V. (1995) Motion of the Earth's center of mass induced by global changes in its dynamic structure and by tidal deformations. Mosc. Univ. Phys. Bull., 1995, 50(5), 92-94. English translation of Vestni. Mosk. Univ. 3, Fiz., Astron. (Russia). 1995, 50(5), 99-101. [2] Barkin Yu.V. (2009) About possible polar drifts of centers of mass of the Earth and Mars. Abstract Book (CD) of European Planetary Science Congress (Potsdam, Germany, 13 - 18 September 2009), Vol.4, EPSC 2009-118. [3] Zotov L.V., Barkin Yu.V., Lubushin A.A. (2008) Geocenter motion and its geodynamical contenst. 'Space Geodynamics and Modeling of the Global Geodynamic Processes'. International scientific conference in the frames of the 'Asian-Pacific Space Geodynamics' Project (APSG 2008). (22-26 September 2008, Novosibirsk, Russian Federation). Abstract book. P. 28 [4] Barkin Yu.V. (2008) Secular polar drift of the core in present epoch: geodynamical and geophysical consequences and confirmations. General and regional problems of tectonics and geodynamics. Materials of XLI Tectonic Conference. V. 1. -M.:GEOS. p. 55-59. In Russian. [5] Barkin Yu.V. (2005) Oscillations of the Earth core, new oceanic tides and dynamical consequences. Materials of XI International Scientific Conference 'Structure, geodynamics and mineral genetic processes in lithosphere' (September, 20-22 2005, Syktyvkar, Russia). Publisher of Geology Institute of Komi SC of Ural Section of RAS, Syktyvkar, pp. 26-28. In Russian. [6] Barkin Yu.V. (2009) An explanation of secular variations of a gravity at stations Ny-Alesund, Medicine, Churchill and Syowa. Materials of the International Conference: «Yu.P. Bulashevich's fifth

  10. Lyapunov analysis: from dynamical systems theory to applications

    Science.gov (United States)

    Cencini, Massimo; Ginelli, Francesco

    2013-06-01

    structures playing a prominent role in the studies, both theoretical and applied, of transport, stirring and mixing properties in fluid flows. This section contains two contributions, one more theoretical in nature and a second with biological applications, where Lagrangian coherent structures and their effect on transport and mixing are analyzed through finite-size Lyapunov exponents. While this special issue, in its very nature, cannot be fully exhaustive, we hope that it will provide a clear and up-to-date picture of the theory and applications of Lyapunov analysis, further stimulating fruitful debate across a number of related research fields. Acknowledgments We would like to acknowledge the Journal of Physics A editorial staff, in particular A Haywood, R Gillan and E O'Callaghan for their continuous assistance which made this special issue possible. References [1] Lorenz E 1993 The Essence of Chaos (Seattle, WA: University of Washington) [2] Poincaré H 1890 Acta Math. 13 1 [3] Poincaré H 1892 Les méthods nouvelles de la mécanique céleste vol 1 (Paris: Gauthier-Villars) Poincaré H 1893 Les méthods nouvelles de la mécanique céleste vol 2 (Paris: Gauthier-Villars) Poincaré H 1899 Les méthods nouvelles de la mécanique céleste vol 3 (Paris: Gauthier-Villars) Poincaré H 1992 New Methods of Celestial Mechanics (New York: American Institute of Physics) (Engl. transl.) [4] Hadamard J 1898 J. Math. Pures Appl. 4 27 [5] van der Pol B 1927 Phil. Mag. 3 65 [6] Fermi E, Pasta J and Ulam S 1955 Studies of nonlinear problems Technical Report LA-1940 (Los Alamos, NM: Los Alamos Scientific Laboratory) [7] Lorenz E N 1963 J. Atmos. Sci. 20 130 [8] Hénon M and Heiles C 1964 Astron. J. 69 73 [9] Kolmogorov A N 1958 Dokl. Akad. Nauk SSSR 119 861 [10] Kolmogorov A 1959 Dokl. Akad. Nauk SSSR 124 754 [11] Chirikov B 1959 At. Energ. 6 630 [12] Smale S 1967 Bull. Am. Math. Soc. 73 747 [13] Ruelle D and Takens F 1971 Commun. Math. Phys. 20 167 [14] Li T Y and Yorke J A 1975 Am. Math

  11. Programa de Pós-Graduação em Geologia - Teses Defendidas 1998 - Doutorado - Instituto de Geociências - Universidade Federal do Rio de Janeiro

    Directory of Open Access Journals (Sweden)

    1998-01-01

    distância, no Morro da Fome. No estado do Rio de Janeiro, temos o sítio arqueológico de Itaboraí, no município do mesmo nome. O sítio está inserido em uma rampa de colúvio situada nos bordos da Bacia Calcária de São José de Itaboraí. 123 Anuário do Instituto de Geociências - UFRJ Volume 21 / 1998 A partir da década de 70 foram utilizados os métodos da relação silte-argila, ferro (Fe livre - ferro (Fe cristalizado, estratigráfico, tipológico e o da correlação geomorfológica (manchas climáticas. O método tipológico revelou uma cadeia tecnológica na confecção dos artefatos cobrindo as técnicas usadas em outras partes do mundo, indo do Pleistoceno Inferior ao Superior, reforçando os resultados obtidos pelos outros métodos relativos. O método absoluto do C14 foi usado à superfície do sítio. Apresentaram-se, também, as vantagens do estudo das manchas climáticas sobre os artefatos para avaliação cronológica. Finalmente, procurou-se através da apresentação dos três casos acima expostos, evidenciar a contribuição do arqueólogo aos estudos do Quaternário. Quanto às pinturas rupestres, sublinhou-se sua validade na interpretação paleoambiental a partir de representações pictóricas de animais pleistocênicos, especialmente em canhões. Utilizou-se o método etnológico-etnográfico para o reconhecimento - a partir de pinturas sobre rochas - de antigas migrações, tomando-se por base mitos, planos cosmológicos, uso de alucinógenos, etc., próprios do grupo lingüístico Tukâno. Essas conclusões foram reforçadas por registros históricos e por estudos no campo da Paleontologia Humana. Finalmente, apresentaram-se dois casos em que o homem préhistórico utilizou extensamente rochas para deixar registrado seu conhecimento astronômico e sua maneira particular de tentar uma integração com o cosmos. Nome: Claudia Guterres Vilela Título: Foraminíferos Quaternários da Plataforma Continental Norte Brasileira e do Leque do