WorldWideScience

Sample records for plages

  1. Pique-nique à la plage.

    Directory of Open Access Journals (Sweden)

    Erwan Le Goff

    2010-02-01

    Full Text Available La plage, domaine public maritime placé sous l’autorité du maire est, a priori, un espace de liberté et d’égalité. Le pouvoir réglementaire de la commune peut cependant agir sur certaines pratiques spatiales, au cœur d’enjeux sociaux et politiques. La plage n’échappe pas à cette réglementation. L’estivant en quête d’un lieu agréable pour pique-niquer à Cabourg se dirigera volontiers vers la plage. La municipalité en a décidé autrement, comme le montre le panneau ...

  2. SOUS LES PAVÉS: LA PLAGE!

    DEFF Research Database (Denmark)

    Clemmensen, Thomas Juel

    2017-01-01

    kunstnerbevægelse situationisterne brugte parolen sous les pavés: la plage! blev stranden associeret med det frie naturlige rum i kontrast til den brolagte gade, der repræsenterede samfundets undertrykkende orden. Men udtrykket kan samtidig minde os om geologiens allestedsnærværende karakter. Geologien findes lige...

  3. Network and plage indices from Kodaikanal Ca-K data

    International Nuclear Information System (INIS)

    Raju, K. P.; Singh, Jagdev

    2014-01-01

    The Ca II K filtergrams from Kodaikanal Solar Observatory have been used to study solar activity. The images are dominated by the chromospheric network and plages. Programs have been developed to obtain the network and plage indices from the daily images as functions of solar latitude and time. Preliminary results from the analysis are reported here. The network and plage indices were found to follow the sunspot cycle. A secondary peak is found during the period of declining activity in both the indices. A comparison of network indices from the northern and the southern hemispheres shows that the former is more active than the latter. However such an asymmetry is not clearly seen in the plage index

  4. Pratiques de la plage en Polynésie française

    Directory of Open Access Journals (Sweden)

    Caroline Blondy

    2014-04-01

    Full Text Available Les plages sont des lieux de coprésence entre touristes et société locale où un double processus d'appropriation territoriale est à l'œuvre. La Polynésie française permet de mettre en évidence les différentes formes de territorialisation entre les plages publiques et les plages privées des hôtels. Les premières connaissent un triple cloisonnement spatial et social des usages de la plage. Elles sont un révélateur de clivages socio-culturels. Quant aux secondes, elles montrent une homogénéité des pratiques et un cloisonnement atténué, posant la question d'une création d'un «entre-soi».

  5. Association of Plages with Sunspots: A Multi-Wavelength Study Using Kodaikanal Ca ii K and Greenwich Sunspot Area Data

    Energy Technology Data Exchange (ETDEWEB)

    Mandal, Sudip; Chatterjee, Subhamoy; Banerjee, Dipankar, E-mail: sudip@iiap.res.in [Indian Institute of Astrophysics, Koramangala, Bangalore 560034 (India)

    2017-02-01

    Plages are the magnetically active chromospheric structures prominently visible in the Ca ii K line (3933.67 Å). A plage may or may not be associated with a sunspot, which is a magnetic structure visible in the solar photosphere. In this study we explore this aspect of association of plages with sunspots using the newly digitized Kodaikanal Ca ii K plage data and the Greenwich sunspot area data. Instead of using the plage index or fractional plage area and its comparison with the sunspot number, we use, to our knowledge for the first time, the individual plage areas and compare them with the sunspot area time series. Our analysis shows that these two structures, formed in two different layers, are highly correlated with each other on a timescale comparable to the solar cycle. The area and the latitudinal distributions of plages are also similar to those of sunspots. Different area thresholdings on the “butterfly diagram” reveal that plages of area ≥4 arcmin{sup 2} are mostly associated with a sunspot in the photosphere. Apart from this, we found that the cyclic properties change when plages of different sizes are considered separately. These results may help us to better understand the generation and evolution of the magnetic structures in different layers of the solar atmosphere.

  6. Evolutionary charts of solar activity (calcium plages) as functions of heliographic longitude and time

    International Nuclear Information System (INIS)

    Hedeman, E.R.; Dodson, H.W.; Roelof, E.C.

    1981-08-01

    The richness and diversity of data relating to solar activity present a challenge from the point of view of organization and evaluation. For phenomena such as plages and centers of activity that tend to last for more than one solar rotation, a sequence of evolutionary charts based on heliographic longitude for successive solar rotations are discussed. Such a diagrammatic representation of calcium plages as a function of longitude and time, coupled with considerations of heliographic latitude, permits relatively easy and confident recognition of successively returning centers of activity

  7. On the relation of Hsub(α) plage brightness variations in solar active regions

    International Nuclear Information System (INIS)

    Ogir', M.B.

    1980-01-01

    The variations of hydrogen plage brightnesses in seven spot groups belonging to five active regions are discussed. The observations were made on the Crimean observatory coronograph in 1974 and 1977. The correlation in brightness variations of plages situated in the regions of growing magnetic field was obtained. This was observed in the plages on one spot group as well as in the different groups removing on about 27x10 4 km. In developed groups correlations are mainly seen within a spot group and they are expressed better during flares. The correlations of brightnesses are changing during the active region evolution. Three days observations showed good brightness correlations of all plages in the growing magnetic field region and their decrease that can be explained by the field weakening during natural active region evolution or by the strong flare influence. The existence of the simultaneous variations of brightness in the regions with the growing magnetic field speaks in favour of the simultaneous carring-out of magnetic field or its disturbances into the chromosphere [ru

  8. Déchets solides encombrants les plages d'Annaba Rabah Chaouch ...

    African Journals Online (AJOL)

    Les rejets des déchets solides sur nos plages constituent une véritable plaie qui dégrade la beauté des paysages. ... Mots clés : environnement; déchets solides; gestion; littoral; santé. Abstract ..... déchets soldes et liquides apportés par les ...

  9. Déchets solides encombrants les plages d'Annaba | Chaouch ...

    African Journals Online (AJOL)

    Nos résultats montrent que les verres et les métaux viennent en 1ère position avec respectivement 32,84% et 32,53 % puis on a les plastiques avec 14,17%, les bois et dérivés 13,88 %, les diverses structures en papier avec 3,32% et enfin les textiles avec 3,26%. La plage Ain-Achir est la plus polluée avec 10,59 Kg/m2 de ...

  10. Scènes de plage dans la peinture hollandaise du XVIIe siècle: l'entrée de la plage dans l'espace des citadins

    Directory of Open Access Journals (Sweden)

    Rémy Knafou

    2000-06-01

    Full Text Available Les scènes de plage sont une catégorie de la peinture hollandaise, inventée au XVIIe siècle. L'analyse d'un corpus de tableaux peints durant le Siècle d’Or permet de montrer que le «désir de rivage» analysé par Alain Corbin est apparu sur le littoral de la mer du Nord dès le XVIIe siècle avec l'ouverture de la plage aux citadins oisifs venus des villes voisines.

  11. SOAP 2.0: a tool to estimate the photometric and radial velocity variations induced by stellar spots and plages

    International Nuclear Information System (INIS)

    Dumusque, X.; Boisse, I.; Santos, N. C.

    2014-01-01

    This paper presents SOAP 2.0, a new version of the Spot Oscillation And Planet (SOAP) code that estimates in a simple way the photometric and radial velocity (RV) variations induced by active regions. The inhibition of the convective blueshift (CB) inside active regions is considered, as well as the limb brightening effect of plages, a quadratic limb darkening law, and a realistic spot and plage contrast ratio. SOAP 2.0 shows that the activity-induced variation of plages is dominated by the inhibition of the CB effect. For spots, this effect becomes significant only for slow rotators. In addition, in the case of a major active region dominating the activity-induced signal, the ratio between the FWHM and the RV peak-to-peak amplitudes of the cross correlation function can be used to infer the type of active region responsible for the signal for stars with v sin i ≤8 km s –1 . A ratio smaller than three implies a spot, while a larger ratio implies a plage. Using the observation of HD 189733, we show that SOAP 2.0 manages to reproduce the activity variation as well as previous simulations when a spot is dominating the activity-induced variation. In addition, SOAP 2.0 also reproduces the activity variation induced by a plage on the slowly rotating star α Cen B, which is not possible using previous simulations. Following these results, SOAP 2.0 can be used to estimate the signal induced by spots and plages, but also to correct for it when a major active region is dominating the RV variation.

  12. SOAP 2.0: a tool to estimate the photometric and radial velocity variations induced by stellar spots and plages

    Energy Technology Data Exchange (ETDEWEB)

    Dumusque, X. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Boisse, I. [Laboratoire d' Astrophysique de Marseille (UMR 6110), Technopole de Château-Gombert, 38 rue Frédéric Joliot-Curie, F-13388 Marseille Cedex 13 (France); Santos, N. C., E-mail: xdumusque@cfa.harvard.edu [Centro de Astrofìsica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto (Portugal)

    2014-12-01

    This paper presents SOAP 2.0, a new version of the Spot Oscillation And Planet (SOAP) code that estimates in a simple way the photometric and radial velocity (RV) variations induced by active regions. The inhibition of the convective blueshift (CB) inside active regions is considered, as well as the limb brightening effect of plages, a quadratic limb darkening law, and a realistic spot and plage contrast ratio. SOAP 2.0 shows that the activity-induced variation of plages is dominated by the inhibition of the CB effect. For spots, this effect becomes significant only for slow rotators. In addition, in the case of a major active region dominating the activity-induced signal, the ratio between the FWHM and the RV peak-to-peak amplitudes of the cross correlation function can be used to infer the type of active region responsible for the signal for stars with v sin i ≤8 km s{sup –1}. A ratio smaller than three implies a spot, while a larger ratio implies a plage. Using the observation of HD 189733, we show that SOAP 2.0 manages to reproduce the activity variation as well as previous simulations when a spot is dominating the activity-induced variation. In addition, SOAP 2.0 also reproduces the activity variation induced by a plage on the slowly rotating star α Cen B, which is not possible using previous simulations. Following these results, SOAP 2.0 can be used to estimate the signal induced by spots and plages, but also to correct for it when a major active region is dominating the RV variation.

  13. Five years of beach drainage survey on a macrotidal beach (Quend-Plage, northern France)

    Science.gov (United States)

    Bain, Olivier; Toulec, Renaud; Combaud, Anne; Villemagne, Guillaume; Barrier, Pascal

    2016-07-01

    A drainage system was installed in 2008 on the macrotidal beach of Quend-Plage, close to Abbeville (Somme, northern France), following a period of significant erosion of recreational areas. The "Direction départementale des territoires et de la mer" (French Coastal Department Authority) has requested a biannual survey in order to validate the beach drainage setup and its efficiency. This paper presents the methodology used for this survey, and the response of the coastal system to this soft engineering method for preventing erosion. These five years of drainage operation have strongly modified the morphology of the beach. Three main modifications occurred: (i) accretion of the upper beach and foredune, (ii) erosion of the lower and middle beach and (iii) a slight shift in directions of the beach bars and troughs. These morphological changes finally led to the stabilization of the beach.

  14. SOAP 2.0: A Tool to Estimate the Photometric and Radial Velocity Variations Induced by Stellar Spots and Plages

    Science.gov (United States)

    Dumusque, X.; Boisse, I.; Santos, N. C.

    2014-12-01

    This paper presents SOAP 2.0, a new version of the Spot Oscillation And Planet (SOAP) code that estimates in a simple way the photometric and radial velocity (RV) variations induced by active regions. The inhibition of the convective blueshift (CB) inside active regions is considered, as well as the limb brightening effect of plages, a quadratic limb darkening law, and a realistic spot and plage contrast ratio. SOAP 2.0 shows that the activity-induced variation of plages is dominated by the inhibition of the CB effect. For spots, this effect becomes significant only for slow rotators. In addition, in the case of a major active region dominating the activity-induced signal, the ratio between the FWHM and the RV peak-to-peak amplitudes of the cross correlation function can be used to infer the type of active region responsible for the signal for stars with v sin i SOAP 2.0 manages to reproduce the activity variation as well as previous simulations when a spot is dominating the activity-induced variation. In addition, SOAP 2.0 also reproduces the activity variation induced by a plage on the slowly rotating star α Cen B, which is not possible using previous simulations. Following these results, SOAP 2.0 can be used to estimate the signal induced by spots and plages, but also to correct for it when a major active region is dominating the RV variation. . The work in this paper is based on observations made with the MOST satellite, the HARPS instrument on the ESO 3.6 m telescope at La Silla Observatory (Chile), and the SOPHIE instrument at the Observatoire de Haute Provence (France).

  15. Influence of the form of the magnetic axis on the regions of stability and their variations (1963); Influence de la forme de l'axe magnetique sur les plages de stabilite et leur variation (1963)

    Energy Technology Data Exchange (ETDEWEB)

    Mercier, C; Tasso, H [Commissariat a l' Energie Atomique, Fontenay-aux-Roses (France). Centre d' Etudes Nucleaires

    1963-07-01

    We study many cases of plane and twisted magnetic axis and we show for a set of regular magnetic axis tending to racetrack limit, the stability regions tend rapidly to the racetrack stability. But, for the case at two axis apparently not very far, we find that the corresponding regions of stability may be sometimes sensibly different. (authors) [French] Nous etudions plusieurs exemples d'axes magnetiques plans et gauches et montrons que pour une suite d'axes magnetiques qui converge vers une limite du type hippodrome, les plages de stabilite convergent rapidement vers la plage limite. Mais, si on prend deux axes apparemment peu eloignes, on trouve que les plages correspondantes peuvent etre parfois sensiblement differentes. (auteurs)

  16. Solar Indices - Plage Regions

    Data.gov (United States)

    National Oceanic and Atmospheric Administration, Department of Commerce — Collection includes a variety of indices related to solar activity contributed by a number of national and private solar observatories located worldwide. This...

  17. Piscines et plages chez Kundera

    DEFF Research Database (Denmark)

    Boisen, Jørn

    2007-01-01

    Swimming pools, stricto sensu, are a newcomer in the gallery of western topoï, linked as they are to 20th century consumer culture. For obvious reasons they have become a recognized cinematographic topos, but - more surprisingly - they have also made their way to novel. For instance you find a lo...... and nihilism in a mode that is much darker and more troubled than one would expect...

  18. SOUS LE PAVÉ: LA PLAGE!

    DEFF Research Database (Denmark)

    Clemmensen, Thomas Juel

    2017-01-01

    of these take their point of departure in the author’s observations of material conditions and processes on the harbor in Aarhus, which highlight the city as a geological phenomenon. But mostly the thoughts are inspired by works and ideas of artists and architects, which more or less consciously have revolved...

  19. La qualité des plages au cœur des enjeux de développement : La situation des îles de l’océan Indien

    Directory of Open Access Journals (Sweden)

    Virginie Duvat

    2009-02-01

    Full Text Available La qualité des plages s’inscrit au cœur des enjeux de développement des petites îles tropicales en raison d’une part, de la place qu’elle occupe dans les stratégies de promotion touristique, et d’autre part, de l’importance que prend le littoral dans les pratiques récréatives et touristiques émergentes des populations locales. Dans ce contexte, l’objectif de cet article est de présenter les résultats d’une évaluation réalisée dans différentes îles des archipels des Seychelles et des Mascareignes, et de mettre en évidence la relation qui existe entre la qualité des plages, leurs attributs naturels et les politiques d’aménagement et de gestion des acteurs publics et privés.Today, the quality of the tropical beaches is closely linked to development challenges for two main reasons. At first, because sandy beaches play an important role in tourism development policies, and secondly because of the emergence of the touristic and recreative activities of the local communities. In this context, the purpose of this paper is to expose the results of an assessment which was done in the Seychelles and Mascarene islands and to highlight the relationship which can be observed between beach quality, natural assets and the strategies of public and private actors.

  20. Short-term evolution and coexistence of spots, plages and flare activity on LQ Hydrae

    Science.gov (United States)

    Flores Soriano, M.; Strassmeier, K. G.

    2017-01-01

    Aims: We aim to study the short-term evolution of the chromospheric and photospheric activity of the young, single K2 dwarf LQ Hya. Methods: Four months of quasi-simultaneous spectroscopic and photometric observations were used to study the variations of the photometric light curve, the evolution of the chromospheric activity from the Hα and Hβ lines, and the distribution of cool spots from Doppler maps. Results: During our observations one side of the star was more active than the other. The equivalent width of the Hα line from the least active hemisphere increased from ≈0.7 Å at the beginning of the observation to 1.0 Å at the end. The basal emission of the most active hemisphere remained roughly constant at EWHαt1.0 Å. Intense flare activity was observed during the first twenty days, where at least four different events were detected. The line asymmetries of the Hα line suggest that one of the flares could have produced a mass ejection with a maximum projected speed of 70kms-1. The rotational modulation of the V-band photometry showed clear anti-correlation with the chromospheric activity. The difference in brightness between the opposite hemispheres decreased from 0.m16 to 0.m09 in two months. Three spots gradually moving apart from each other are dominating the photospheric Doppler maps. The comparison between the maps and the Hα line as the star rotates reveals the spatial coexistence of chromospheric Hα emission and photospheric spots. Conclusions: Our results indicate that the active regions of LQ Hya can live for at least four months. The detected changes in the photometric light curve and the spectroscopic Doppler images seem to be more a consequence of the spatial redistribution of the active regions rather than due to changes in their strength. Only one of the active regions shows significant changes in its chromospheric emission. Based on data obtained with the STELLA robotic telescope in Tenerife, an AIP facility jointly operated by AIP and IAC, and the Vienna-Potsdam Automatic Photoelectric Telescopes at Fairborn Observatory in Arizona, operated by AIP.

  1. Schrödinger à la plage la physique quantique dans un transat

    CERN Document Server

    Antoine, Charles

    2018-01-01

    Née au début du XXème siècle, la physique quantique décrit un monde bizarre, celui de l'infiniment petit, et ses effets à notre échelle sont encore mal compris. Erwin Schrödinger en est une figure emblématique. Il a participé à presque toutes les étapes clé et son équation décrivant l'évolution dans le temps d'une particule, critiquée par Einstein qui pensait que Dieu ne joue pas aux dés, est devenue l'un des piliers de la mécanique quantique. Aujourd'hui, la physique quantique est partout dans notre quotidien, du smartphone au GPS, en passant par l'imagerie médicale. Elle nous offrira demain de nouvelles applications, tels l'ordinateur ou la téléportation quantiques. Installez-vous confortablement dans un transat, et laissez-vous conter par Charles Antoine l'étrangeté du monde quantique. Mais attention, si le voyage est fabuleux, vous n'en ressortirez pas indemne...

  2. Déchets solides encombrants les plages d'Annaba Rabah Chaouch ...

    African Journals Online (AJOL)

    Rachid, Rizi amor, la caroube, Réfés zahouan, Belvédère et Ain Achir. Après avoir photographié les sites à l'aide d'un appareil à photographier numérique ..... 3. la mise en œuvre d'une stratégie qui développe les activités de recyclage - valorisation par un système de reprise, de recyclage et de valorisation des déchets et.

  3. Erika: evaluation of residual sanitary risks linked to the beaches-going after cleaning-up; Erika: evaluation des risques sanitaires residuels lies a la frequentation des plages apres depollution

    Energy Technology Data Exchange (ETDEWEB)

    NONE

    2000-07-01

    The aim of this study is to evaluate the sanitary risks for the populations frequenting the coast beaches affected by the fuel oils of the tanker Erika, after their cleaning up. This quantitative evaluation of sanitary risks is led according to a protocol developed jointly between the two institutes ( the national institute of industrial environment and risks, I.N.E.R.I.S., and the national institute of sanitary watch I.n.V.S.). It does not give the risks in function the residual pollution level of concerned beaches but supplies to the authorities elements of scientific information in order to allow them to choose criteria appropriate for the management of eventual residual risks. (N.C.)

  4. Evaluation of the residual sanitary risk for people spending time on the beaches polluted by the Erika fuel, after the depollution; Evaluation du risque sanitaire residuel pour les populations frequentant les plages polluees par le fioul rejete par l'ERIKA, apres depollution

    Energy Technology Data Exchange (ETDEWEB)

    Dor, F.; Gourier-Frery, C.; Zmirou, D. [Institut de veille sanitaire, 94 - Saint-Maurice (France); Cicolella, A.; Bonnard, R.; Dujardin, R. [Institut National de l' Environnement Industriel et des Risques, 60 - Verneuil en Halatte (INERIS) (France)

    2004-07-01

    This study aims to evaluate the short dated and long dated sanitary risks for adults and children who are going to spend time on the beach affected by the Erika fuel, after the depollution. 36 beaches were selected and 7 beaches which were not polluted, were taking as a reference. The methodology, the analysis of the data and the results are described. (A.L.B.)

  5. Dosimetry evaluation of the potential exposure bound to uranium and thorium natural accumulation in the sand of some beaches of the Camargue littoral; Evaluations dosimetriques de l'exposition potentielle liee a l'accumulation naturelle d'uranium et de thorium dans les sables de certaines plages du littoral de Camargue

    Energy Technology Data Exchange (ETDEWEB)

    NONE

    2007-07-01

    The aim of this report is the assessment of potential exposure to radioactive sands discovered in 2000 in two points of the coast of the Camargue (East of Beauduc and Espiguette lighthouses), where specific activity can reach up several thousands of Bq.kg{sup -1} for radionuclides of U{sup 238} and Th{sup 232} radioactive families, and environmental dose rate up to ten times of usual natural background. The excess of radioactivity is carried by small particles of sand (apatites and zircons less than 100 {mu}m). First chapter focuses on radioactivity of the coast of the Golfe du lion and of the Camargue, and more particularly on these two points (cartography, measure, radionuclide identification, mineralogical characterization of particles). This chapter concludes the excess of radioactivity is natural; particles come from several massifs of the Rhone basin, transported by the river and re-distributed on the coast. Second chapter focuses on dosimetric assessment, using reasonable scenarios for the frequenting of these sites by persons of the public in one hand, and drawing up the sizing of the sands and their solubility in gastric and intestinal fluids in an other hand. the annual effective dose, carefully calculated, is about 1 mSv, mainly due to external exposure to gamma rays. such a dose, of same levels as the dose received for 17 months of residence in Paris for example, does not involve any particular action. (authors)

  6. Unusual Large-Scale Flaring Structure

    National Research Council Canada - National Science Library

    Chertok, I

    2002-01-01

    .... The transient originated at a relatively small middle-latitude soft X-ray bright point (XBP), which was also visible in the EUV range and had a small underlying Halpha plage with a bipolar magnetic configuration...

  7. A Butterfly Diagram and Carrington Maps for Century-long CA II K Spectroheliograms from The Kodaikanal Observatory

    Science.gov (United States)

    Chatterjee, Subhamoy; Banerjee, Dipankar; Ravindra, B.

    2016-08-01

    The century-long (1907-2007) Ca II K spectroheliograms from the Kodaikanal Solar Observatory (KSO) are calibrated, processed, and analyzed to follow the evolution of the bright on-disc structures called plages, possible representatives of magnetic activity on the Sun. This is the longest data set studied in Ca II K to date, covering about 9.5 cycles of 11 yr periods. Plages are segmented with area ≥slant 1 {{arcmin}}2 using global thresholds for individual full disc images and subsequent application of a morphological closing operation. The plage index is calculated and is seen to have a close positive correlation with the fractional disc area covered by plages. The newly generated plage area cycle (from KSO) was compared with the same from the Mount Wilson Observatory (correlation 95.6%) for the overlapping years, I.e., 1915-2000. This study illustrates the time-latitude distribution of plage centroids by rendering a butterfly diagram (as observed for sunspots). The 3D visualization of the diagram shows one-to-one mapping between plage location, time, and area. This work further delineates the positional correlation between magnetic patches and plage regions through the comparison of synoptic maps derived from both KSO Ca II K images and space-based full disc line-of-sight magnetograms. Regular synoptic magnetograms from ground-based observatories are available only after 1970s. Thus the long term Ca II K data from KSO can be used as a proxy for estimating magnetic activity locations and their strengths at earlier times.

  8. Estimation des changements de la ligne de rivage de la zone côtière ...

    African Journals Online (AJOL)

    Les plages du littoral de Kénitra ont connu des modifications au cours de ces quatre dernières décennies. La mise en valeur économique de certaines plages par des aménagements touristiques et l'extraction massive de sables pour les travaux d'aménagements urbains sont à l'origine d'une déstabilisation des échanges ...

  9. Répartition et abondance des sargasses Sargassum natans et ...

    African Journals Online (AJOL)

    Ces plantes se retrouvent en abondance en mai et en juin sur toutes les plages du pays et particulièrement sur les plages du secteur littoral centre et oriental et les complexes lagunaires Aby-Tendo-Ehy et Grand-Lahou. Leur expansion en mai dans tous les milieux est favorisée par la salinité, la lumière, la température et ...

  10. Steady flows in the chromosphere and transition-zone above active regions as observed by OSO-8

    Science.gov (United States)

    Lites, B. W.

    1980-01-01

    Two years of data from the University of Colorado ultraviolet spectrometer aboard OSO-8 were searched for steady line-of-sight flows in the chromosphere and transition-zone above active regions. The most conspicuous pattern that emerges from this data set is that many sunspots show persistent blueshifts of transition-zone lines indicating velocities of about 20 km/s with respect to the surrounding plage areas. The data show much smaller shifts in ultraviolet emission lines arising from the chromosphere: the shifts are frequently to the blue, but sometimes redshifts do occur. Plage areas often show a redshift of the transition-zone lines relative to the surrounding quiet areas, and a strong gradient of the vertical component of the velocity is evident in many plages. One area of persistent blueshift was observed in the transition-zone above an active region filament. The energy requirement of these steady flows over sunspots is discussed.

  11. Decree D.G.S./.A. no. 2003/166 of the 2. april 2003 relative to the definition of beaches opening conditions following the pollution of the atlantic littoral by petroleum products and to the specific measures to implement during the holidays season 2003; Circulaire DGS/SD7A no. 2003/166 du 2 avril 2003 relative a la definition des conditions d'ouverture des plages a la suite de la pollution du littoral atlantique par des produits petroliers et aux mesures specifiques a mettre en oeuvre durant la saison balneaire 2003

    Energy Technology Data Exchange (ETDEWEB)

    NONE

    2003-04-15

    The present decree sets the mode of sanitary monitoring of coastal zones polluted by the release of petroleum products following the sinking of the 'Prestige' petroleum ship in 2002. It specifies the cleanness criteria of beaches after the remedial action and the information toward the public. (N.C.)

  12. SOAP 2.0: Spot Oscillation And Planet 2.0

    Science.gov (United States)

    Dumusque, Xavier; Boisse, I.; Santos, N. C.

    2015-04-01

    SOAP (Spot Oscillation And Planet) 2.0 simulates the effects of dark spots and bright plages on the surface of a rotating star, computing their expected radial velocity and photometric signatures. It includes the convective blueshift and its inhibition in active regions.

  13. Spatially Resolved Images and Solar Irradiance Variability R ...

    Indian Academy of Sciences (India)

    Abstract. The Sun is the primary source of energy that governs both the terrestrial climate and near-earth space environment. Variations in UV irradiances seen at earth are the sum of global (solar dynamo) to regional. (active region, plage, network, bright points and background) solar mag- netic activities that can be ...

  14. 419-420

    Indian Academy of Sciences (India)

    tribpo

    locations of sunspots with strong magnetic fields and at the locations of plages having larger areas. Presented here are the results of an analysis of intensity of green line emission and the active region magnetic signatures as seen in Stanford magnetograms. The data base used in this study consisted of homogeneous data ...

  15. Modeling Li I and K I sensitivity to Pleiades activity

    NARCIS (Netherlands)

    Stuik, R.; Bruls, J.H.M.J.; Rutten, R.J.

    1996-01-01

    We compare schematic modeling of spots and plage on the surface of cool dwarfs with Pleiades data to assess effects of magnetic activity on the strengths of the L II and K I resonance lines in Pleiades spectra. Comprehensive L II and K I NLTE line formation computation is combined with comparatively

  16. DEVELOPEMENT OF A LIGHT ATTENUATOR BASED ON GLASSY ...

    African Journals Online (AJOL)

    30 juin 2012 ... d'atténuation réel variant de 63% à l'extinction dans une plage angulaire de 0 à 70°. 5. RÉFÉRENCES. [1] Jeong Y. S., Bae S. C., Jung Y., Oh K. Micro-optical waveguide on micro-actuating platform and its application in variable optical attenuator. Optical Fiber Technology. 2006, 12, 38– 47. Laser.

  17. A MURI Center for Intelligent Biomimetic Image Processing and Classification

    Science.gov (United States)

    2007-11-01

    times, labeled "plage" or "open space" or "natural", the system learns to associate multiple classes with a given input. Testbed image examples have shown...brain color perception and category learning. Commentary on "Coordinating perceptually grounded categories through language " by Luc Steels and Tony...Symposium on Computational Intelligence (ISCI), Kosice, Slovakia, June 2002. 9. Carpenter, G.A., Award from the Slovak Artificial Intelligence Society, 2002

  18. diversité botanique dans le sud du parc national de taï, côte d

    African Journals Online (AJOL)

    AKA Boko Mathieu

    Résumé. L'analyse globale de la croissance de trois espèces d'algues rouges ; Hypnea musciformis, Gracilaria multipartita et Gelidium sesquipedale a été entreprise dans le but de déterminer la variabilité interspécifique au sein du même milieu naturel. Le site étudié est la plage de Mehdia située au nord de la côte ...

  19. Some results of model calculations of the solar S-component radio emission

    International Nuclear Information System (INIS)

    Krueger, A.; Hildebrandt, J.

    1985-01-01

    Numerical calculations of special characteristics of the solar S-component microwave radiation are presented on the basis of recent sunspot and plage models. Quantitative results are discussed and can be used for the plasma diagnostics of solar active regions by comparisons with observations with high spatial and spectral resolution. The possibility of generalized applications to magnetic stars and stellar activity is briefly noted. (author)

  20. Contribution à l'étude de la radioactivité gamma du sable des ...

    African Journals Online (AJOL)

    Les familles de l'Uranium -238, de l'Uranium -235, du Thorium -232 et du Potassium -40 sont d'origines telluriques et contribuent de manière générale aux expositions internes et externes d'un individu. Ce travail a pour objectif de mesurer la radioactivité du sable de deux plages de la baie de Diego-Suarez, à savoir celles ...

  1. Contribution à la connaissance de la faune marine de la region d'Arcachon

    NARCIS (Netherlands)

    Lacourt, A.W.

    1977-01-01

    INTRODUCTION Le matériel qui constitue le sujet de cet article a été rassemblé pendant une vingtaine d'années, depuis 1956, sur la plage d'Arcachon et de Cap Ferret. Des recherches ont été faites sur les deux côtes de la langue de terre de Cap Ferret et à quelques endroits aux alentours d'Arcachon.

  2. Analyse de la croissance de Gymnogongrus patens Agardh de la ...

    African Journals Online (AJOL)

    Rhodophyta, Phyllophoraceae) a été analysée sur des échantillons d'algues récoltés mensuellement pendant un cycle annuel, d'avril 2002 à mars 2003, sur la plage de Méhdia (Nord ouest de la côte atlantique marocaine). L'analyse des paramètres de ...

  3. Imaging capabilities of SXT for Solar-A

    Science.gov (United States)

    Lemen, J. R.; Acton, L. W.; Brown, W. A.; Bruner, M. E.; Catura, R. C.

    1991-01-01

    The present study characterizes the Soft X-ray Telescope (SXT), a grazing-incidence solar X-ray telescope which will be flown on the Japanese Solar-A satellite. X-ray tests showed that the SXT mirror meets or exceeds design requirements. SXT advantages over Skylab are: improved time resolution (not less than 0.5 s), greatly decreased mirror scatter, coaligned aspect telescope to intersperse images of sunspots and magnetic plage, and digital data readout.

  4. CHROMOSPHERIC HEATING BY ACOUSTIC WAVES COMPARED TO RADIATIVE COOLING

    Energy Technology Data Exchange (ETDEWEB)

    Sobotka, M.; Heinzel, P.; Švanda, M.; Jurčák, J. [Astronomical Institute, Academy of Sciences of the Czech Republic (v.v.i.), Fričova 298, 25165 Ondřejov (Czech Republic); Del Moro, D.; Berrilli, F. [Department of Physics, University of Roma Tor Vergata, Via della Ricerca Scientifica 1, I-00133 Rome (Italy)

    2016-07-20

    Acoustic and magnetoacoustic waves are among the possible candidate mechanisms that heat the upper layers of the solar atmosphere. A weak chromospheric plage near the large solar pore NOAA 11005 was observed on 2008 October 15, in the Fe i 617.3 nm and Ca ii 853.2 nm lines of the Interferometric Bidimemsional Spectrometer attached to the Dunn Solar Telescope. In analyzing the Ca ii observations (with spatial and temporal resolutions of 0.″4 and 52 s) the energy deposited by acoustic waves is compared to that released by radiative losses. The deposited acoustic flux is estimated from the power spectra of Doppler oscillations measured in the Ca ii line core. The radiative losses are calculated using a grid of seven one-dimensional hydrostatic semi-empirical model atmospheres. The comparison shows that the spatial correlation of the maps of radiative losses and acoustic flux is 72%. In a quiet chromosphere, the contribution of acoustic energy flux to radiative losses is small, only about 15%. In active areas with a photospheric magnetic-field strength between 300 and 1300 G and an inclination of 20°–60°, the contribution increases from 23% (chromospheric network) to 54% (a plage). However, these values have to be considered as lower limits and it might be possible that the acoustic energy flux is the main contributor to the heating of bright chromospheric network and plages.

  5. Solar spectral irradiance variability of some chromospheric emission lines through the solar activity cycles 21-23

    Directory of Open Access Journals (Sweden)

    Göker Ü.D.

    2017-01-01

    Full Text Available A study of variations of solar spectral irradiance (SSI in the wave-length ranges 121.5 nm-300.5 nm for the period 1981-2009 is presented. We used various data for ultraviolet (UV spectral lines and international sunspot number (ISSN from interactive data centers such as SME (NSSDC, UARS (GDAAC, SORCE (LISIRD and SIDC, respectively. We reduced these data by using the MATLsoftware package. In this respect, we revealed negative correlations of intensities of UV (289.5 nm-300.5 nm spectral lines originating in the solar chromosphere with the ISSN index during the unusually prolonged minimum between the solar activity cycles (SACs 23 and 24. We also compared our results with the variations of solar activity indices obtained by the ground-based telescopes. Therefore, we found that plage regions decrease while facular areas are increasing in SAC 23. However, the decrease in plage regions is seen in small sunspot groups (SGs, contrary to this, these regions in large SGs are comparable to previous SACs or even larger as is also seen in facular areas. Nevertheless, negative correlations between ISSN and SSI data indicate that these variations are in close connection with the classes of sunspots/SGs, faculae and plage regions. Finally, we applied the time series analysis of spectral lines corresponding to the wavelengths 121.5 nm-300.5 nm and made comparisons with the ISSN data. We found an unexpected increase in the 298.5 nm line for the Fe II ion. The variability of Fe II ion 298.5 nm line is in close connection with the facular areas and plage regions, and the sizes of these solar surface indices play an important role for the SSI variability, as well. So, we compared the connection between the sizes of faculae and plage regions, sunspots/SGs, chemical elements and SSI variability. Our future work will be the theoretical study of this connection and developing of a corresponding model.

  6. 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

  7. Photometric measurements of solar irradiance variations due to sunspots

    International Nuclear Information System (INIS)

    Chapman, G.A.; Herzog, A.D.; Laico, D.E.; Lawrence, J.K.; Templer, M.S.

    1989-01-01

    A photometric telescope constructed to obtain photometric sunspot areas and deficits on a daily basis is described. Data from this Cartesian full disk telescope (CFDT) are analyzed with attention given to the period between June 4 and June 17, 1985 because of the availability of overlapping sunspot area and irradiance deficit data from high-resolution digital spectroheliograms made with the San Fernando Observatory 28 cm vacuum solar telescope and spectroheliograph. The CFDT sunspot deficits suggest a substantial irradiance contribution from faculae and active region plage. 23 refs

  8. SPATIAL DISTRIBUTIONS OF ABSORPTION, LOCAL SUPPRESSION, AND EMISSIVITY REDUCTION OF SOLAR ACOUSTIC WAVES IN MAGNETIC REGIONS

    International Nuclear Information System (INIS)

    Chou, D.-Y.; Yang, M.-H.; Zhao Hui; Liang Zhichao; Sun, M.-T.

    2009-01-01

    Observed acoustic power in magnetic regions is lower than the quiet Sun because of absorption, emissivity reduction, and local suppression of solar acoustic waves in magnetic regions. In the previous studies, we have developed a method to measure the coefficients of absorption, emissivity reduction, and local suppression of sunspots. In this study, we go one step further to measure the spatial distributions of three coefficients in two active regions, NOAA 9055 and 9057. The maps of absorption, emissivity reduction, and local suppression coefficients correlate with the magnetic map, including plage regions, except the emissivity reduction coefficient of NOAA 9055 where the emissivity reduction coefficient is too weak and lost among the noise.

  9. Outflow of chromospheric emission features from the rim of a sunspot

    Science.gov (United States)

    Liu, S.-Y.

    1973-01-01

    In viewing a 16 mm movie made from a time sequence of spectroheliograms, some of these emission features are found to move outward from the rim of the sunspot until they are eventually lost in the small plage. There are two interpretations for the streaming of the magnetic features. It is possible that kinks in the line of force propagate along a horizontal extension of the penumbral magnetic field. Alternatively, fragments of the sunspot magnetic field are carried away by the photospheric velocity field.

  10. Study of the Effect of Active Regions on the Scattering Polarization in the Solar Corona

    Science.gov (United States)

    Derouich, M.; Badruddin

    2018-03-01

    The solar photospheric/chromospheric light exciting atoms/ions is not homogeneous because of the presence of active regions (ARs). The effect of ARs on the scattering polarization at the coronal level is an important ingredient for a realistic determination of the magnetic field. This effect is usually disregarded or mixed with other effects in the sense that the degree of its importance is not well known. The aim of this paper is to study the effect of atmospheric inhomogeneities on the coronal scattering polarization. We determined quantitatively the importance of the atmospheric inhomogeneities by using given geometries of solar ARs (plages and sunspots).

  11. The Soft X-ray Telescope for Solar-A - Design evolution and lessons learned

    Science.gov (United States)

    Bruner, Marilyn E.

    1992-01-01

    The Japanese Solar-A satellite mission's Soft X-ray Telescope uses grazing-incidence optics, a CCD detector, and a pair of filter wheels for wavelength selection. A coaxially-mounted visible-light lens furnished sunspot and magnetic plage images, together with aspect information which aids in aligning the soft X-ray images with those from the satellite's Hard X-ray Telescope. Instrument electronics are microprocessor-based, and imbedded in a tightly integrated distributed system. Control software is divided between the instrument microprocessor and the spacecraft control computer.

  12. Investigation of possible sun-weather relationships

    International Nuclear Information System (INIS)

    Businger, S.

    1978-01-01

    Statistical correlations between anomalous solar activity (as denoted by large solar flares, active plages, and interplanetary magnetic sector boundaries) and the circulation of the troposphere are reviewed. Two indices (measuring atmospheric vorticity and mean zonal geostrophic flow in the northern hemisphere) are analyzed in an effort to reveal possible sun-weather relationships. The result of this analysis provides no additional statistical evidence for a connection between solar activity and the weather. Finally, physical mechanisms that have been suggested to explain the claimed correlations are discussed

  13. 101 Aspects macroscopiques de la reproduction de Engraulis ...

    African Journals Online (AJOL)

    HP 630

    Résumé. Les aspects macroscopiques de la reproduction de l'anchois Engraulis encrasicolus ont été étudiés de janvier 2014 à décembre 2014. Les spécimens proviennent de la pêche artisanale le long du littoral-ouest de la Côte d'Ivoire. Les échantillonnages ont été réalisés avec les sennes de plage et les sennes ...

  14. Les trous noirs

    CERN Document Server

    Ioli, Elena

    2016-01-01

    L'univers est peuplé par des étoiles, des planètes, des galaxies, des astéroïdes, des comètes, mais les trous noirs en sont certainement les habitants les plus mystérieux et les plus fascinants ! Grâce à cette merveilleuse histoire racontée par papy Gino, professeur d'astronomie, les trous noirs n auront plus de secrets pour vous ! C est l'été, le soleil illumine le ciel, la plage est en feu : une journée à la plage pleine de jeux et de plongée qui va se transformer pour Bernardo, Gregorio et leurs deux amis en une aventure inattendue. Ils découvriront les secrets des trous noirs, d étranges objets célestes que personne n'a jamais vus mais qui existent bel et bien ! Grand-père Gino, un professeur d astronomie à la retraite, emmènera les enfants à l'intérieur d'un trou noir, leur expliquera pourquoi ils sont noirs, comment ils sont nés et comment les scientifiques pensent qu'ils vont mourir. Et Gino leur racontera même ce qui se trouve de l'autre côté d'un trou noir...

  15. Soap, A Free-code Tool To Study The Impact Of Stellar Activity

    Science.gov (United States)

    Boisse, Isabelle; Bonfils, X.; Santos, N.

    2011-09-01

    Dark spots and bright plages are present on the surface of all stars, even low-active stars (like the Sun in its low-active phase). Their appearance and disappearance on the stellar photosphere, combined with the stellar rotation, may lead to errors and uncertainties in the characterization of planets both in radial velocimetry and photometry. SOAP is a tool offered to the community (Boisse, Bonfils and Santos, in prep.) that enables to simulate spots and plages on rotating stars and computes their impact on RV and photometric measurements. This talk will discuss the challenges related to the knowledge of stellar activity for the next decade: detect telluric planets in the habitable zone of their stars (from G to M dwarfs), understand the activity in the low-mass end of M dwarf (on which will focus future projects like Elektra, SPIRou or CARMENES), limitation to the sum of different transit observations in order to characterize the atmospheric components (from the ground or with Spitzer, JWST), planets around young stars,... and how this can be simulated with SOAP in order to search for indices and corrections. IB and NCS would like to thank the support by the European Research Council/European Community under the FP7 through a Starting Grant, as well from Fundacao para a Ciencia e a Tecnologia (FCT), Portugal.

  16. SOAP: A Tool for the Fast Computation of Photometry and Radial Velocity Induced by Stellar Spots

    Science.gov (United States)

    Boisse, I.; Bonfils, X.; Santos, N. C.; Figueira, P.

    2013-04-01

    Dark spots and bright plages are present on the surface of dwarf stars from spectral types F to M, even in their low-active phase (like the Sun). Their appearance and disappearance on the stellar photosphere, combined with the stellar rotation, may lead to errors and uncertainties in the characterization of planets both in radial velocity (RV) and photometry. Spot Oscillation and Planet (SOAP) is a tool offered to the community that enables to simulate spots and plages on rotating stars and computes their impact on RV and photometric measurements. This tool will help to understand the challenges related to the knowledge of stellar activity for the next decade: detect telluric planets in the habitable zone of their stars (from G to M dwarfs), understand the activity in the low-mass end of M dwarf (on which future projects, like SPIRou or CARMENES, will focus), limitation to the characterization of the exoplanetary atmosphere (from the ground or with Spitzer, JWST), search for planets around young stars. These can be simulated with SOAP in order to search for indices and corrections to the effect of activity.

  17. TIME DEPENDENT NONEQUILIBRIUM IONIZATION OF TRANSITION REGION LINES OBSERVED WITH IRIS

    Energy Technology Data Exchange (ETDEWEB)

    Martínez-Sykora, Juan; Pontieu, Bart De; Hansteen, Viggo H. [Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA 94304 (United States); Gudiksen, Boris, E-mail: j.m.sykora@astro.uio.no [Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, NO-0315 Oslo (Norway)

    2016-01-20

    The properties of nonstatistical equilibrium ionization of silicon and oxygen ions are analyzed in this work. We focus on five solar targets (quiet Sun; coronal hole; plage; quiescent active region, AR; and flaring AR) as observed with the Interface Region Imaging Spectrograph (IRIS). IRIS is best suited for this work owing to the high cadence (up to 0.5 s), high spatial resolution (up to 0.″32), and high signal-to-noise ratios for O iv λ1401 and Si iv λ1402. We find that the observed intensity ratio between lines of three times ionized silicon and oxygen ions depends on their total intensity and that this correlation varies depending on the region observed (quiet Sun, coronal holes, plage, or active regions) and on the specific observational objects present (spicules, dynamic loops, jets, microflares, or umbra). In order to interpret the observations, we compare them with synthetic profiles taken from 2D self-consistent radiative MHD simulations of the solar atmosphere, where the statistical equilibrium or nonequilibrium treatment of silicon and oxygen is applied. These synthetic observations show vaguely similar correlations to those in the observations, i.e., between the intensity ratios and their intensities, but only in the nonequilibrium case do we find that (some of) the observations can be reproduced. We conclude that these lines are formed out of statistical equilibrium. We use our time-dependent nonequilibrium ionization simulations to describe the physical mechanisms behind these observed properties.

  18. Canoë-Kayak Club

    CERN Multimedia

    Canoë-Kayak Club

    2012-01-01

    Mobilisation Initiatives Océanes.   Pour la deuxième année consécutive, le Canoë Kayak CERN s’est mobilisé pour soutenir l’action de la fondation Surfrider en participant aux Initiatives Océanes qui se déroulent chaque année au début du printemps pour lutter contre les déchets qui polluent nos océans, plages, lacs et rivières. En 2011, cela représentait dans le monde 40’000 participants, 7’500 scolaires, 34 pays et plus de 950 nettoyages. Le Canoë kayak CERN a souhaité poursuivre l’action mené en 2011, de la Jonction (à Genève) jusqu’au Lignon, en continuant de nettoyer les berges du Rhône du Lignon jusqu’au port d’Aire-la-Ville et la plage de Peney, avec une équipe sur l'eau, en cano...

  19. Removing Activity-Related Radial Velocity Noise to Improve Extrasolar Planet Searches

    Science.gov (United States)

    Saar, Steven; Lindstrom, David M. (Technical Monitor)

    2004-01-01

    We have made significant progress towards the proposal goals of understanding the causes and effects of magnetic activity-induced radial velocity (v_r) jitter and developing methods for correcting it. In the process, we have also made some significant discoveries in the fields of planet-induced stellar activity, planet detection methods, M dwarf convection, starspot properties, and magnetic dynamo cycles. We have obtained super high resolution (R approximately 200,000), high S / N (greater than 300) echelle study of joint line bisector and radial velocity variations using the McDonald 2-D coude. A long observing run in October 2002 in particular was quite successful (8 clear nights). We now have close to three years of data, which begins to sample a good fraction of the magnetic cycle timescales for some of our targets (e.g., kappa Ceti; P_cyc = 5.6 yrs). This will be very helpful in unraveling the complex relationships between plage and radial velocity (v-r) changes which we have uncovered. Preliminary analysis (Saar et al. 2003) of the data in hand, reveals correlations between median line bisector displacement and v_r. The correlation appears to be specific the the particular star being considered, probably since it is a function of both spectral type and rotation rate. Further analysis and interpretation will be in the context of evolving plage models and is in progress.

  20. Disentangling stellar activity from exoplanetary signals with interferometry

    Directory of Open Access Journals (Sweden)

    Ligi Roxanne

    2015-01-01

    Full Text Available Stellar activity can express as many forms at stellar surfaces: dark spots, convective cells, bright plages. Particularly, dark spots and bright plages add noise on photometric data or radial velocity measurements used to detect exoplanets, and thus lead to false detection or disrupt their derived parameters. Since interferometry provides a very high angular resolution, it may constitute an interesting solution to distinguish the signal of a transiting exoplanet and that of stellar activity. It has also been shown that granulation adds bias in visibility and closure phase measurements, affecting in turn the derived stellar parameters. We analyze the noises generated by dark spots on interferometric observables and compare them to exoplanet signals. We investigate the current interferometric instruments able to measure and disentangle these signals, and show that there is a lack in spatial resolution. We thus give a prospective of the improvements to be brought on future interferometers, which would also significantly extend the number of available targets.

  1. A REESTRUTURAÇÃO PRODUTIVA E O CIRCUITO INFERIOR DO TURISMO NAS PRAIAS DE REDINHA NOVA, SANTA RITA E JENIPABU, EXTREMOZ – RN

    Directory of Open Access Journals (Sweden)

    José Alexandre Berto de Almada

    2017-03-01

    Cette étude vise à analyser le processus de restructuration productive du tourisme à Rio Grande do Norte du territoire utilisée par le circuit inférieur du tourisme sur les plages appartenant à APAJ, Redinha Nova, Santa Rita et Jenipabu dans la municipalité de Extremoz, afin de comprendre la relation dialectique de l'interdépendance entre dépendante circuit inférieur du tourisme dans ces plages et le circuit supérieur fait du tourisme dans la Via Costeira et plage de Ponta Negra à Natal. L'analyse du circuit inférieur a été réalisée à partir du travail de terrain, effectué entre Janvier et Juin 2014 dans l’APAJ, qui a interviewé presque tous les commerçants locaux, à l'exception des dix entreprises ou des commerçants fermés qui ont refusé de participer à l'entrevue, totalisant quatre-vingt dix six établissements visités. Au cours du travail sur le terrain, nous avons également recueilli des données cartographiques via l'unité GPS dans laquelle ils ont été utilisés dans la préparation des cartes de répartition spatiale de l'urbanisation et territoire utilisés par le circuit inférieur dans l’APAJ. Lors de la visite de la ville de NatalLes touristes ne sont pas seulement dans cette ville. Il existe une variété de lieux à visiter, à la fois sur la côte nord et la côte sud de Rio Grande do Norte. L'un de ces lieux sont les plages de l’APAJ, Redinha Nova, Santa Rita et Jenipabu où le processus d'urbanisation dans la Via Costeira et Ponta Negra rendu possible la mise en place du circuit touristique inférieur cette apa. L'afflux de touristes à ces plages apporte avec elle un discours de développement économique pour le lieu et pour les habitants. La contradiction entre les deux circuits est plus mauvais pour ceux qui sont sur le côté inférieur de l'économie. Alors que les entreprises du circuit supérieur visent l'accumulation de capital ainsi que les dividendes peuvent être utilisés dans de nouveaux

  2. Comments on filament-disintegration and its relation to other aspects of solar activity.

    Science.gov (United States)

    Dodson, H. W.; Hedeman, E. R.; Rovira De Miceli, M.

    1972-01-01

    Studies of sudden disintegrations of filaments in solar cycles 19 and 20 (to 1969) indicate that such events occur frequently. Approximately 30% of all large filaments in these cycles disintegrated in the course of their transit across the solar disk. 'Major' flares occurred with above average frequency on the last day on which 141 large disappearing filaments were observed. Relationships between a disintegrating filament on July 10-11, 1959, a prior major flare, a newly formed spot, and concomitant growth of H-alpha plage are presented. Observation of prior descending prominence material apparently directed towards the location of the flare of July 15, 1959 is reported. The development of the filament-associated flare of Feb. 13, 1967 is described.

  3. IRAS observations of chromospherically active dwarf stars

    Science.gov (United States)

    Tsikoudi, Vassiliki

    1989-01-01

    Far-infrared observations of chromospherically active, spotted, and plage stars in the dF7-dk7 spectral range are examined. Most (75 percent) of the stars have detectable 12-micron fluxes, and 50 percent of them have 25-micron emission. The 12-micron luminosity, L(12), is found to be in the range of 1.5-13 x 10 to the 30th ergs/s and to comprise only 0.2-0.5 percent of the star's total luminosity, L(bol). The present work extends to earlier spectral types and higher stellar luminosities the L(12) vs L(bol) relationship noted previously for late-type active dwarfs (K5-M5).

  4. IRAS observations of chromospherically active dwarf stars

    Energy Technology Data Exchange (ETDEWEB)

    Tsikoudi, V. (Ioannina Univ. (Greece))

    1989-07-01

    Far-infrared observations of chromospherically active, spotted, and plage stars in the dF7-dk7 spectral range are examined. Most (75 percent) of the stars have detectable 12-micron fluxes, and 50 percent of them have 25-micron emission. The 12-micron luminosity, L(12), is found to be in the range of 1.5-13 x 10 to the 30th ergs/s and to comprise only 0.2-0.5 percent of the star's total luminosity, L(bol). The present work extends to earlier spectral types and higher stellar luminosities the L(12) vs L(bol) relationship noted previously for late-type active dwarfs (K5-M5). 17 refs.

  5. Atmospheric activity in red dwarf stars

    International Nuclear Information System (INIS)

    Pettersen, B.R.

    1986-01-01

    Active and inactive stars of similar mass and luminosity have similar physical conditions in their photospheres, outside of magnetically disturbed regions. Such field structures give rise to stellar activity, which manifests itself at all heights of the atmosphere. Observations of uneven distributions of flux across the stellar disc have led to the disovery of photospheric starspots, chromospheric plage areas, and coronal holes. Localized transient behavior has been identified in both thermal and non-thermal sources, such as flares, shock waves and particle acceleration. The common element to all active regions is the presence of strong magnetic field structures connecting the violently turbulent deep layers in the convection zones of stars with the tenuous outer atmospheres. Transport and dissipation of energy into the chromospheric and coronal regions are still much debated topics

  6. 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

  7. Les Mayas à Hollywood.

    Directory of Open Access Journals (Sweden)

    Boris Jeanne

    2007-02-01

    Full Text Available Les Mayas de nos jours ce sont surtout des grandes pyramides au milieu de la forêt à un jet d’avion de Cancún : pour nombre de touristes américains et européens, c’est une occasion de s’acoquiner avec la culture, la grande culture des civilisations perdues, en continuant de boire des piña coladas le soir au bord de la plage. Et puis au mois de décembre les Mayas ont débarqué en force dans le paysage culturel local des Américains et des Européens, dans leurs cinémas, au moyen de deux films in...

  8. Energy balance in solar and stellar chromospheres

    Science.gov (United States)

    Avrett, E. H.

    1981-01-01

    Net radiative cooling rates for quiet and active regions of the solar chromosphere and for two stellar chromospheres are calculated from corresponding atmospheric models. Models of chromospheric temperature and microvelocity distributions are derived from observed spectra of a dark point within a cell, the average sun and a very bright network element on the quiet sun, a solar plage and flare, and the stars Alpha Boo and Lambda And. Net radiative cooling rates due to the transitions of various atoms and ions are then calculated from the models as a function of depth. Large values of the net radiative cooling rate are found at the base of the chromosphere-corona transition region which are due primarily to Lyman alpha emission, and a temperature plateau is obtained in the transition region itself. In the chromospheric regions, the calculated cooling rate is equal to the mechanical energy input as a function of height and thus provides a direct constraint on theories of chromospheric heating.

  9. Absorption of acoustic waves by sunspots. II - Resonance absorption in axisymmetric fibril models

    Science.gov (United States)

    Rosenthal, C. S.

    1992-01-01

    Analytical calculations of acoustic waves scattered by sunspots which concentrate on the absorption at the magnetohydrodynamic Alfven resonance are extended to the case of a flux-tube embedded in a uniform atmosphere. The model is based on a flux-tubes of varying radius that are highly structured, translationally invariant, and axisymmetric. The absorbed fractional energy is determined for different flux-densities and subphotospheric locations with attention given to the effects of twist. When the flux is highly concentrated into annuli efficient absorption is possible even when the mean magnetic flux density is low. The model demonstrates low absorption at low azimuthal orders even in the presence of twist which generally increases the range of wave numbers over which efficient absorption can occur. Resonance absorption is concluded to be an efficient mechanism in monolithic sunspots, fibril sunspots, and plage fields.

  10. Joaquín Sorolla pintor del Rey Alfonso XIII 

    Directory of Open Access Journals (Sweden)

    Jordane Fauvey

    2011-06-01

    Full Text Available « Aujourd’hui Sorolla intéresse », déclarait Florencio de Santa-Ana, directeur du Musée Sorolla de Madrid, à l’occasion de l’exposition Sorolla íntimo (2004. En effet, depuis les années 1980-90, le peintre des plages de Valence est à la mode. En témoignent la fréquence des expositions concernant directement son œuvre, ou encore le prix des toiles qui sont aujourd’hui les plus élevées du marché, juste derrière les chef-d’œuvres des impressionnistes français. Ces dernières années ont également...

  11. Perfection of the individual photographic emulsion dosimeter; Perfectionnements dans la dosimetrie individuelle par emulsion photographique

    Energy Technology Data Exchange (ETDEWEB)

    Soudain, G [Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    A photographic dosimeter making possible the measurement of {gamma} radiation doses of from 10 mr up to 800 r by means of 3 emulsion bands of varying sensitivity stuck to the same support is described. The dosimeter has also a zone for marking and a test film insensitive to radiation. This requires a photometric measurement by diffuse reflection an d makes it possible to measure doses with an accuracy of 20 per cent. (author) [French] On decrit un dosimetre photographique permettant la mesure des doses de rayonnement {gamma} depuis 10 mroentgens jusqu'a 800 roentgens, au moyen de trois bandes d'emulsions de sensibilites differentes collees sur le meme support. Le dosimetre comporte egalement une plage de marquage et un temoin de developpement insensibles au rayonnement. Ceci impose la mesure photometrique par reflexion diffuse et permet l'appreciation visuelle des doses a 20 pour cent pres. (auteur)

  12. Magnetohydrodynamic waves driven by p-modes

    International Nuclear Information System (INIS)

    Khomenko, Elena; Santamaria, Irantzu Calvo

    2013-01-01

    Waves are observed at all layers of the solar atmosphere and the magnetic field plays a key role in their propagation. While deep down in the atmosphere the p-modes are almost entirely of acoustic nature, in the upper layers magnetic forces are dominating, leading to a large variety of new wave modes. Significant advances have been made recently in our understanding of the physics of waves interaction with magnetic structures, with the help of analytical theories, numerical simulations, as well as high-resolution observations. In this contribution, we review recent observational findings and current theoretical ideas in the field, with an emphasis on the following questions: (i) Peculiarities of the observed wave propagation in network, plage and facular regions; (ii) Role of the mode transformation and observational evidences of this process: (iii) Coupling of the photosphere, chromosphere, and above by means of waves propagating in magnetic structures.

  13. Galite

    OpenAIRE

    Soumille, P.

    2012-01-01

    La Galite est une île située par 37°31’ de latitude Nord et 8’55’ de longitude Est, au large de la côte septentrionale de la Tunisie, à 25 milles marins (46 kilomètres) au Nord du Cap Negro, à 33 milles (61 kilomètres) au Nord/Nord-Est de Tabarka et à 50 milles (92 kilomètres) au Nord/Nord-Ouest de la rade de Bizerte. Les Instructions nautiques sur les côtes de Tunisie, datant de 1890, nous décrivent ainsi l’île : « C’est un gros massif de terre escarpé et sans plage de trois milles de longue...

  14. XSST/TRC rocket observations of July 13, 1982 flare. [X-ray Spectrometer, Spectrograph and Telescope/Transition Region Camera

    Science.gov (United States)

    Foing, Bernard H.; Bonnet, Roger M.; Dame, Luc; Bruner, Marilyn; Acton, Loren W.

    1986-01-01

    The present analysis of UV filtergrams of the July 13, 1982 solar flare obtained by the XSST/TRC rocket experiments has used calibrated intensities of the flare components to directly estimate the Lyman-alpha line flux, C IV line flux, and excess 160-nm continuum temperature brighness over the underlying plage. The values obtained are small by comparison with other observed or calculated equivalent quantities from the Machado (1980) model of flare F1. The corresponding power required to heat up to the temperature minimum over the 1200 sq Mm area is found to be 3.6 x 10 to the 25th erg/sec for this small X-ray C6 flare, 7 min after the ground-based observed flare maximum.

  15. XSST/TRC rocket observations of July 13, 1982 flare

    International Nuclear Information System (INIS)

    Foing, B.H.; Bonnet, R.M.; Dame, L.; Bruner, M.; Acton, L.W.

    1986-01-01

    The present analysis of UV filtergrams of the July 13, 1982 solar flare obtained by the XSST/TRC rocket experiments has used calibrated intensities of the flare components to directly estimate the Lyman-alpha line flux, C IV line flux, and excess 160-nm continuum temperature brighness over the underlying plage. The values obtained are small by comparison with other observed or calculated equivalent quantities from the Machado (1980) model of flare F1. The corresponding power required to heat up to the temperature minimum over the 1200 sq Mm area is found to be 3.6 x 10 to the 25th erg/sec for this small X-ray C6 flare, 7 min after the ground-based observed flare maximum. 13 references

  16. Helium emission in the middle chromosphere

    International Nuclear Information System (INIS)

    Livshits, M.A.

    1976-01-01

    Slitless spectrograms obtained during the eclipse of 10 June 1972 have been analyzed to determine the height distribution of the D 3 He line intensity. For undisturbed regions the maximum of D 3 line intensity is confirmed to exist at about 1700 km above the limb. Besides the above mentioned maximum, in plages a considerable intensity may be observed at low heights (h 1000 km has been carried out within the low temperature mechanism of triplet helium emission taking into account the helium ionization by XUV radiation. The density dependence of the 2 3 S level population at different XUV flux values has been calculated. The observations give Nsub(e) approximately 2x10 10 cm -3 in the chromosphere at h = 2000 km. The probable coincidence of the H and He emission small filaments in the middle chromosphere is discussed. (Auth.)

  17. HELIOSEISMIC SIGNATURE OF CHROMOSPHERIC DOWNFLOWS IN ACOUSTIC TRAVEL-TIME MEASUREMENTS FROM HINODE

    International Nuclear Information System (INIS)

    Nagashima, Kaori; Sekii, Takashi; Kosovichev, Alexander G.; Zhao Junwei; Tarbell, Theodore D.

    2009-01-01

    We report on a signature of chromospheric downflows in two emerging flux regions detected by time-distance helioseismology analysis. We use both chromospheric intensity oscillation data in the Ca II H line and photospheric Dopplergrams in the Fe I 557.6 nm line obtained by Hinode/SOT for our analyses. By cross-correlating the Ca II oscillation signals, we have detected a travel-time anomaly in the plage regions; outward travel times are shorter than inward travel times by 0.5-1 minute. However, such an anomaly is absent in the Fe I data. These results can be interpreted as evidence of downflows in the lower chromosphere. The downflow speed is estimated to be below 10 km s -1 . This result demonstrates a new possibility of studying chromospheric flows by time-distance analysis.

  18. HARPS-N OBSERVES THE SUN AS A STAR

    Energy Technology Data Exchange (ETDEWEB)

    Dumusque, Xavier; Glenday, Alex; Phillips, David F.; Charbonneau, David; Latham, David W.; Li, Chih-Hao; Sasselov, Dimitar; Szentgyorgyi, Andrew; Walsworth, Ronald [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Buchschacher, Nicolas; Lovis, Christophe; Pepe, Francesco; Udry, Stéphane [Observatoire Astronomique de l’Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny (Switzerland); Cameron, Andrew Collier [SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY16 9SS (United Kingdom); Cecconi, Massimo; Cosentino, Rosario; Ghedina, Adriano; Lodi, Marcello; Molinari, Emilio, E-mail: xdumusque@cfa.harvard.edu [INAF—Fundación Galileo Galilei, Rambla José Ana Fernández Pérez 7, E-38712 Breña Baja (Spain)

    2015-12-01

    Radial velocity (RV) perturbations induced by stellar surface inhomogeneities including spots, plages and granules currently limit the detection of Earth-twins using Doppler spectroscopy. Such stellar noise is poorly understood for stars other than the Sun because their surface is unresolved. In particular, the effects of stellar surface inhomogeneities on observed stellar radial velocities are extremely difficult to characterize, and thus developing optimal correction techniques to extract true stellar radial velocities is extremely challenging. In this paper, we present preliminary results of a solar telescope built to feed full-disk sunlight into the HARPS-N spectrograph, which is in turn calibrated with an astro-comb. This setup enables long-term observation of the Sun as a star with state-of-the-art sensitivity to RV changes. Over seven days of observing in 2014, we show an average 50 cm s{sup −1} RV rms over a few hours of observation. After correcting observed radial velocities for spot and plage perturbations using full-disk photometry of the Sun, we lower by a factor of two the weekly RV rms to 60 cm s{sup −1}. The solar telescope is now entering routine operation, and will observe the Sun every clear day for several hours. We will use these radial velocities combined with data from solar satellites to improve our understanding of stellar noise and develop optimal correction methods. If successful, these new methods should enable the detection of Venus over the next two to three years, thus demonstrating the possibility of detecting Earth-twins around other solar-like stars using the RV technique.

  19. Five-minute oscillation power within magnetic elements in the solar atmosphere

    International Nuclear Information System (INIS)

    Jain, Rekha; Gascoyne, Andrew; Hindman, Bradley W.; Greer, Benjamin

    2014-01-01

    It has long been known that magnetic plage and sunspots are regions in which the power of acoustic waves is reduced within the photospheric layers. Recent observations now suggest that this suppression of power extends into the low chromosphere and is also present in small magnetic elements far from active regions. In this paper we investigate the observed power suppression in plage and magnetic elements, by modeling each as a collection of vertically aligned magnetic fibrils and presuming that the velocity within each fibril is the response to buffeting by incident p modes in the surrounding field-free atmosphere. We restrict our attention to modeling observations made near the solar disk center, where the line-of-sight velocity is nearly vertical and hence, only the longitudinal component of the motion within the fibril contributes. Therefore, we only consider the excitation of axisymmetric sausage waves and ignore kink oscillations as their motions are primarily horizontal. We compare the vertical motion within the fibril with the vertical motion of the incident p mode by constructing the ratio of their powers. In agreement with observational measurements we find that the total power is suppressed within strong magnetic elements for frequencies below the acoustic cut-off frequency. However, further physical effects need to be examined for understanding the observed power ratios for stronger magnetic field strengths and higher frequencies. We also find that the magnitude of the power deficit increases with the height above the photosphere at which the measurement is made. Furthermore, we argue that the area of the solar disk over which the power suppression extends increases as a function of height.

  20. Nature urbaine et urbanité dans la station touristique de Salou (Espagne, au travers de l’étude : d’un parc-promenade, d’un paseo, d’un parc urbain

    Directory of Open Access Journals (Sweden)

    Jean Rieucau

    2010-11-01

    Full Text Available Les espaces publics naturés deviennent un enjeu de l’attractivité touristique des stations côtières sur le littoral méditerranéen espagnol. Les municipalités conduisent des politiques de récupération urbaine sur les plages, les hauts de plage, le long du linéaire côtier, aux dépens d’une urbanisation anarchique, héritée des années 1960 (hôtels, terrains de camping. Les paysagistes confrontés aux clivages entre la ville touristique et la ville « habitante » utilisent une végétation allogène, décontextualisée (palmiers, pour les espaces publics mis en tourisme et recourent à une nature indigène (oliviers, cyprès pour les espaces communs des résidents permanents.The forested public areas become a stake of the touristic appeal of coastal destinations on the Mediterranean coast of Spain. The municipalities steer the urban recovery policies on the beaches, beach heights, along the coastal line, at the expense of anarchical urbanization, inherited from the years 1960 (hotels, camping ground. The landscapers, confronted with the split between touristic city and “resident” city, use exotic vegetation, out of context (palm tree for public areas developed into tourism, and resort to indigenous nature (olive trees, cypress for common areas for the permanent residents.

  1. Radial-Velocity Signatures of Magnetic Features on the Sun Observed as a Star

    Science.gov (United States)

    Palumbo, M. L., III; Haywood, R. D.; Saar, S. H.; Dupree, A. K.; Milbourne, T. W.

    2017-12-01

    In recent years, the search for Earth-mass planets using radial-velocity measurements has become increasingly limited by signals arising from stellar activity. Individual magnetic features induce localized changes in intensity and velocity, which combine to change the apparent radial velocity of the star. Therefore it is critical to identify an indicator of activity-driven radial-velocity variations on the timescale of stellar rotation periods. We use 617.3 nm photospheric filtergrams, magnetograms, and dopplergrams from SDO/HMI and 170.0 nm chromospheric filtergrams from AIA to identify magnetically-driven solar features and reconstruct the integrated solar radial velocity with six samples per day over the course of 2014. Breaking the solar image up into regions of umbrae, penumbrae, quiet Sun, network, and plages, we find a distinct variation in the center-to-limb intensity-weighted velocity for each region. In agreement with past studies, we find that the suppression of convective blueshift is dominated by plages and network, rather than dark photospheric features. In the future, this work will be highly useful for identifying indicators which correlate with rotationally modulated radial-velocity variations. This will allow us to break the activity barrier that currently precludes the precise characterization of exoplanet properties at the lowest masses. This work was supported by the NSF-REU solar physics program at SAO, grant number AGS-1560313. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute.

  2. A First Comparison of Millimeter Continuum and Mg ii Ultraviolet Line Emission from the Solar Chromosphere

    Energy Technology Data Exchange (ETDEWEB)

    Bastian, T. S. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 (United States); Chintzoglou, G.; De Pontieu, B.; Schmit, D. [Lockheed Martin Solar and Astrophysics Lab, Org. A021S, Building 252, 3251 Hanover Street, Palo Alto, CA 94304 (United States); Shimojo, M. [National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588 (Japan); Leenaarts, J. [Institute for Solar Physics, Department of Astronomy, Stockholm University, AlbaNova University Centre, SE-106 91 Stockholm (Sweden); Loukitcheva, M., E-mail: tbastian@nrao.edu [Center For Solar-Terrestrial Research, New Jersey Institute of Technology, 323 Martin Luther King Boulevard, Newark, NJ 07102 (United States)

    2017-08-20

    We present joint observations of the Sun by the Atacama Large Millimeter/submillimeter Array (ALMA) and the Interface Region Imaging Spectrograph ( IRIS ). Both millimeter/submillimeter- λ continuum emission and ultraviolet (UV) line emission originate from the solar chromosphere and both have the potential to serve as powerful and complementary diagnostics of physical conditions in this enigmatic region of the solar atmosphere. The observations were made of a solar active region on 2015 December 18 as part of the ALMA science verification effort. A map of the Sun’s continuum emission was obtained by ALMA at a wavelength of 1.25 mm (239 GHz). A contemporaneous map was obtained by IRIS in the Mg ii h doublet line at 2803.5 Å. While a clear correlation between the 1.25 mm brightness temperature T{sub B} and the Mg ii h line radiation temperature T {sub rad} is observed, the slope is <1, perhaps as a result of the fact that these diagnostics are sensitive to different parts of the chromosphere and that the Mg ii h line source function includes a scattering component. There is a significant difference (35%) between the mean T{sub B} (1.25 mm) and mean T {sub rad} (Mg ii). Partitioning the maps into “sunspot,” “quiet areas,” and “plage regions” we find the relation between the IRIS Mg ii h line T {sub rad} and the ALMA T {sub B} region-dependent. We suggest this may be the result of regional dependences of the formation heights of the IRIS and ALMA diagnostics and/or the increased degree of coupling between the UV source function and the local gas temperature in the hotter, denser gas in plage regions.

  3. A First Comparison of Millimeter Continuum and Mg ii Ultraviolet Line Emission from the Solar Chromosphere

    International Nuclear Information System (INIS)

    Bastian, T. S.; Chintzoglou, G.; De Pontieu, B.; Schmit, D.; Shimojo, M.; Leenaarts, J.; Loukitcheva, M.

    2017-01-01

    We present joint observations of the Sun by the Atacama Large Millimeter/submillimeter Array (ALMA) and the Interface Region Imaging Spectrograph ( IRIS ). Both millimeter/submillimeter- λ continuum emission and ultraviolet (UV) line emission originate from the solar chromosphere and both have the potential to serve as powerful and complementary diagnostics of physical conditions in this enigmatic region of the solar atmosphere. The observations were made of a solar active region on 2015 December 18 as part of the ALMA science verification effort. A map of the Sun’s continuum emission was obtained by ALMA at a wavelength of 1.25 mm (239 GHz). A contemporaneous map was obtained by IRIS in the Mg ii h doublet line at 2803.5 Å. While a clear correlation between the 1.25 mm brightness temperature T_B and the Mg ii h line radiation temperature T _r_a_d is observed, the slope is <1, perhaps as a result of the fact that these diagnostics are sensitive to different parts of the chromosphere and that the Mg ii h line source function includes a scattering component. There is a significant difference (35%) between the mean T_B (1.25 mm) and mean T _r_a_d (Mg ii). Partitioning the maps into “sunspot,” “quiet areas,” and “plage regions” we find the relation between the IRIS Mg ii h line T _r_a_d and the ALMA T _B region-dependent. We suggest this may be the result of regional dependences of the formation heights of the IRIS and ALMA diagnostics and/or the increased degree of coupling between the UV source function and the local gas temperature in the hotter, denser gas in plage regions.

  4. Rôle des additifs anti-usure des huiles lubrifiantes dans un teste de frottement simulant le contact segment-chemise Role of Antiwear Additives for Lube Oils in a Friction Test Simulating Ring-Liner Contact

    Directory of Open Access Journals (Sweden)

    Martin J. M.

    2006-11-01

    Full Text Available Nous avons mis en oeuvre un test de frottement dans lequel les conditions tribologiques sont voisines de celles existant au niveau segment-chemise des moteurs à explosion. Nous avons éprouvé différentes huiles commerciales ainsi que des additifs purs. Ayant choisi la température comme paramètre variable au cours de ce test nous pouvons déterminer pour chaque lubrifiant une plage de température correspondant à une zone d'efficacité maximale de l'additif anti-usure qu'il contient. La température correspondant à la limite inférieure de cette plage est liée à la nature chimique de l'additif. De plus lorsqu'un gradient de température existe entre les deux pièces en frottement, on observe, dans la zone d'efficacité maximale du lubrifiant, un phénomène de pulsations verticales de la goutte d'huile placée dans le contact. Des éléments d'interprétation, expliquant ces deux phénomènes, sont proposés et conduisent à relier l'efficacité anti-usure d'un additif à ses propriétés d'adsorption à la surface des pièces frottantes. The tribological conditions in the test used were similar to these existing in the ringliner area. of explosion engines. Different commercial cils were tested along with pure additives. Since temperature was chosen as a variable parameter during these tests, it was possible to determine a temperature range for each lubricant, corresponding to the maximum efficiency zone for the antiwear additive it contained. The temperature corresponding to the lower limit of this range is linked to the chemical nature of the additive. Likewise, when a temperature gradient exists between two rubbing parts, a vertical pulsation phenomenon of the drop of cil n the contact area occurs in the maximum efficiency zone of the lubricant. Interpretation elements explaining these two phenomena are proposed and lead to linking the antiwear efficiency of an additive to its adsorption properties on the surface of rubbing parts.

  5. Effect of Diffuser and Volute on Turbocharger Centrifugal Compressor Stability and Performance: Experimental Study Effet du diffuseur et de la volute sur la performance et la stabilité d’un compresseur centrifuge de suralimentation: étude expérimentale

    Directory of Open Access Journals (Sweden)

    Mohtar H.

    2011-11-01

    Full Text Available Engine downsizing is potentially one of the most effective strategies being explored to improve fuel economy. A main problem of downsizing using a turbocharger is the small range of stable functioning of the turbocharger centrifugal compressor at high boost pressures. Several techniques were studied to increase the compressor operating range without sacrificing the compressor efficiency. This paper presents the effect of delaying diffuser stability on the compressor performance and surge line. Two different techniques were investigated, these are grooved and pinched diffuser. Moreover, the effect on retracting volute tongue on compressor performance is also studied. Pinched diffuser shifted surge line to low flow rates, while dropping pressure through compressor. On the other hand, some interesting results were obtained when using grooved diffuser, these are pressure increase at high flow rates, and choke line shift to high flow rates. While retracting volute tongue was interesting in improving compressor efficiency, and pressure lines at high speed. Le “downsizing” moteur est potentiellement l’une des stratégies les plus efficaces pour baisser la consommation carburant. Un problème majeur du “downsizing” à l’aide d’un turbocompresseur est la petite plage de fonctionnement stable du compresseur centrifuge à haute pression de suralimentation. Plusieurs techniques ont été étudiées pour augmenter la plage de fonctionnement du compresseur, sans sacrifier le rendement du compresseur. Cet article présente l’effet de la stabilisation du diffuseur sur la performance du compresseur et la ligne de pompage. Deux techniques différentes ont été étudiées, les sillons et le pincement diffuseur. De plus, l’effet de la diminution du bec de la volute sur les performances du compresseur a également été étudié. Le pincement du diffuseur a déplacé la ligne de pompage pour de faibles débits. Ce déplacement a été accompagn

  6. Star-spot distributions and chromospheric activity on the RS CVn type eclipsing binary SV Cam

    Science.gov (United States)

    Şenavcı, H. V.; Bahar, E.; Montes, D.; Zola, S.; Hussain, G. A. J.; Frasca, A.; Işık, E.; Yörükoǧlu, O.

    2018-06-01

    Using a time series of high-resolution spectra and high-quality multi-colour photometry, we reconstruct surface maps of the primary component of the RS CVn type rapidly rotating eclipsing binary, SV Cam (F9V + K4V). We measure a mass ratio, q, of 0.641(2) using our highest quality spectra and obtain surface brightness maps of the primary component, which exhibit predominantly high-latitude spots located between 60° - 70° latitudes with a mean filling factor of ˜35%. This is also indicated by the R-band light curve inversion, subjected to rigourous numerical tests. The spectral subtraction of the Hα line reveals strong activity of the secondary component. The excess Hα absorption detected near the secondary minimum hints to the presence of cool material partially obscuring the primary star. The flux ratios of Ca II IRT excess emission indicate that the contribution of chromospheric plage regions associated with star-spots is dominant, even during the passage of the filament-like absorption feature.

  7. Cine-Club

    CERN Multimedia

    Cine-Club

    2011-01-01

    Lundi 12 décembre 2011 à 18:30 Salle du Conseil Comme chaque année avant Noël, le CINE-CLUB du CERN est heureux d’inviter petits et grands à une projection gratuite du film : Ponyo sur la falaise (Japon, 2008, Hayao Miyazaki) Le petit Sosuke vit avec sa mère sur une haute falaise surplombant la mer. Un beau jour, il découvre sur la plage caillouteuse Ponyo, une petite fille poisson. Ponyo est si fascinée par Sosuke et le monde terrestre que son désir le plus cher est de devenir un être humain. Mais Fujimoto, son magicien de père, n’est pas du tout d’accord avec cette idée et il la force à regagner les profondeurs de l’océan. Bien décidée à revoir Sosuke, Ponyo s’échappe de sa prison sous-marine, mais ce faisant elle déclenche une immense catastroph...

  8. Radio stars observed in the LAMOST spectral survey

    Science.gov (United States)

    Zhang, Li-Yun; Yue, Qiang; Lu, Hong-Peng; Han, Xian-Ming L.; Zhang, Yong; Shi, Jian-Rong; Wang, Yue-Fei; Hou, Yong-Hui; Zi-Huang, Cao

    2017-09-01

    Radio stars have attracted astronomers’ attention for several decades. To better understand the physics behind stellar radio emissions, it is important to study their optical behaviors. The LAMOST survey provides a large database for researching stellar spectroscopic properties of radio stars. In this work, we concentrate on their spectroscopic properties and infer physical properties from their spectra, such as stellar activity and variability. We mined big data from the LAMOST spectral survey Data Release 2 (DR2), published on 2016 June 30, by cross-matching them with radio stars from FIRST and other surveys. We obtained 783 good stellar spectra with high signal to noise ratio for 659 stars. The criteria for selection were positional coincidence within 1.5‧‧ and LAMOST objects classified as stars. We calculated the equivalent widths (EWs) of the Ca ii H&K, Hδ, Hγ, Hβ, Hα and Ca ii IRT lines by integrating the line profiles. Using the EWs of the Hα line, we detected 147 active stellar spectra of 89 objects having emissions above the Hα continuum. There were also 36 objects with repeated spectra, 28 of which showed chromospheric activity variability. Furthermore, we found 14 radio stars emitting noticeably in the Ca ii IRT lines. The low value of the EW8542/EW8498 ratio for these 14 radio stars possibly alludes to chromospheric plage regions.

  9. A statistical study of current-sheet formation above solar active regions based on selforganized criticality

    Science.gov (United States)

    Dimitropoulou, M.; Isliker, H.; Vlahos, L.; Georgoulis, M.; Anastasiadis, A.; Toutountzi, A.

    2013-09-01

    We treat flaring solar active regions as physical systems having reached the self-organized critical state. Their evolving magnetic configurations in the low corona may satisfy an instability criterion, related to the excession of a specific threshold in the curl of the magnetic field. This imposed instability criterion implies an almost zero resistivity everywhere in the solar corona, except in regions where magnetic-field discontinuities and. hence, local currents, reach the critical value. In these areas, current-driven instabilities enhance the resistivity by many orders of magnitude forming structures which efficiently accelerate charged particles. Simulating the formation of such structures (thought of as current sheets) via a refined SOC cellular-automaton model provides interesting information regarding their statistical properties. It is shown that the current density in such unstable regions follows power-law scaling. Furthermore, the size distribution of the produced current sheets is best fitted by power laws, whereas their formation probability is investigated against the photospheric magnetic configuration (e.g. Polarity Inversion Lines, Plage). The average fractal dimension of the produced current sheets is deduced depending on the selected critical threshold. The above-mentioned statistical description of intermittent electric field structures can be used by collisional relativistic test particle simulations, aiming to interpret particle acceleration in flaring active regions and in strongly turbulent media in astrophysical plasmas. The above work is supported by the Hellenic National Space Weather Research Network (HNSWRN) via the THALIS Programme.

  10. Catalog of solar particle events 1955--1969

    International Nuclear Information System (INIS)

    Anon.

    1975-01-01

    This catalog, which is a common enterprise of solar physicists and space scientists, consists of three parts. The first part contains a complete list of 732 particle events of solar origin recorded at the Earth or in space from the first PCA observation in 1955 up to the end of 1969; it thus covers two solar cycle maxima. Each particle event is described in detail by using many unpublished data, kindly made available by more than 20 space scientists. A group of solar experts has tried to look up the source, or alternative sources, of each particle event on the Sun. These sources (with estimates of ''certainty'') are presented, and all the flares which have been considered to be obvious or probable sources of the particle events are summarized in the second part of the catalog, with a description of their characteristic features in the optical, radio, and X-ray spectral range. Finally, the third part describes the active regions in which these flares occurred, including magnetic field maps, plage and sunspot group configurations, flare positions (often with flare photographs), data on the active region development, and bibliography

  11. SOAP. A tool for the fast computation of photometry and radial velocity induced by stellar spots

    Science.gov (United States)

    Boisse, I.; Bonfils, X.; Santos, N. C.

    2012-09-01

    We define and put at the disposal of the community SOAP, Spot Oscillation And Planet, a software tool that simulates the effect of stellar spots and plages on radial velocimetry and photometry. This paper describes the tool release and provides instructions for its use. We present detailed tests with previous computations and real data to assess the code's performance and to validate its suitability. We characterize the variations of the radial velocity, line bisector, and photometric amplitude as a function of the main variables: projected stellar rotational velocity, filling factor of the spot, resolution of the spectrograph, linear limb-darkening coefficient, latitude of the spot, and inclination of the star. Finally, we model the spot distributions on the active stars HD 166435, TW Hya and HD 189733, which reproduce the observations. We show that the software is remarkably fast, allowing several evolutions in its capabilities that could be performed to study the next challenges in the exoplanetary field connected with the stellar variability. The tool is available at http://www.astro.up.pt/soap

  12. The Physics and Diagnostic Potential of Ultraviolet Spectropolarimetry

    Science.gov (United States)

    Trujillo Bueno, Javier; Landi Degl'Innocenti, Egidio; Belluzzi, Luca

    2017-09-01

    The empirical investigation of the magnetic field in the outer solar atmosphere is a very important challenge in astrophysics. To this end, we need to identify, measure and interpret observable quantities sensitive to the magnetism of the upper chromosphere, transition region and corona. This paper provides an overview of the physics and diagnostic potential of spectropolarimetry in permitted spectral lines of the ultraviolet solar spectrum, such as the Mg ii h and k lines around 2800 Å, the hydrogen Lyman-α line at 1216 Å, and the Lyman-α line of He ii at 304 Å. The outer solar atmosphere is an optically pumped vapor and the linear polarization of such spectral lines is dominated by the atomic level polarization produced by the absorption and scattering of anisotropic radiation. Its modification by the action of the Hanle and Zeeman effects in the inhomogeneous and dynamic solar atmosphere needs to be carefully understood because it encodes the magnetic field information. The circular polarization induced by the Zeeman effect in some ultraviolet lines (e.g., Mg ii h & k) is also of diagnostic interest, especially for probing the outer solar atmosphere in plages and more active regions. The few (pioneering) observational attempts carried out so far to measure the ultraviolet spectral line polarization produced by optically pumped atoms in the upper chromosphere, transition region and corona are also discussed. We emphasize that ultraviolet spectropolarimetry is a key gateway to the outer atmosphere of the Sun and of other stars.

  13. Observing the Sun with Coronado telescopes telescopes

    CERN Document Server

    Pugh, Philip

    2007-01-01

    The Sun provides amateur astronomers with one of the few opportunities for daytime astronomy. In order to see the major features of our nearest star, special telescopes that have a very narrow visible bandwidth are essential. The bandwidth has to be as narrow as 1 A- 10-10 m (1 Angstrom) and centred on the absorption line of neutral hydrogen. This makes many major features of the Suna (TM)s chromosphere visible to the observer. Such narrow-band "Fabry-Perot etalon filters" are high technology, and until the introduction of the Coronado range of solar telescopes, were too expensive for amateur use. The entry-level Coronado telescope, the PST (Personal Solar Telescope) costs under 500. Solar prominences (vast columns of plasma, best seen at the edge of the solar disk), filaments, flares, sunspots, plage and active regions are all visible and can be imaged to produce spectacular solar photographs. Philip Pugh has assembled a team of contributors who show just how much solar work can be done with Coronado telesco...

  14. Nouveaux pétroles : quel avenir ? Partie 2 New Oil: What's in the Future? Part Two

    Directory of Open Access Journals (Sweden)

    Boy De la Tour X.

    2006-11-01

    Full Text Available PaL'accroissement des prix de 1973 a rendu accessible toute une plage de pétroles chers, mais ces nouveaux pétroles soulèvent encore des problèmes techniques considérables et leur compétitivité économique a été très affectée par le retournement du marché pétrolier. Quel est l'état des technologies ? Que reste-t-il des ambitieux projets conçus dans les années 70 ? Aux horizons 2000/2010, quel sera l'impact de ces nouveaux pétroles, en terme de quantités et au plan stratégique ? Telles sont les questions auxquelles la présente étude tente de répondre. The increase in oil prices in 1973 made an entire range of expensive oil available, but this new oil still raises considerable technical problems, and its economic competitiveness has been greatly affected by the downturn in the oil market. What is the state of the art of existing technologies ? What remains of the ambitious projects conceived in the 1970s? As of 2000/2010, what will the impact of this new oil be in terms of amounts and from the strategic standpoint? These are the questions that the present study attempts to answer.

  15. A mechanism for solar ultraviolet flux variability

    International Nuclear Information System (INIS)

    Schatten, K.H.; Heath, D.F.

    1981-01-01

    Solar UV emission observed by a filter photometer on Nimbus IV from 1969 to 1973 is examined in an attempt to understand the short term (27 day) and secular variability. Two models are discussed to explain the variations - a calcium plage model and a chromospheric network (faculae and spicule) structure model. Both relate to the remnant magnetic fields of active regions. An association between UV brightenings and the large scale magnetic field has been found consistent with the network model. An increase in UV emittance can be achieved by raising the effective chromospheric temperature closer to a photospheric level. If the Sun's luminosity is constant on these time intervals the enhanced UV radiation could be partially offset by an overall decrease in photospheric temperature as measured by Livingston in visible photospheric profiles. Total solar luminosity may then show less variability, however, the UV to visible luminosity variation may have significant planetary influences. Lockwood and Thompson (1979) report a relation between solar activity and planetary albedos, and Schatten (1979) discussed a long-suspected relationship between solar activity and the Great Red Spot appearance. (orig.)

  16. Atypical aetiology of a conjugal fever: autochthonous airport malaria between Paris and French Riviera: a case report

    Directory of Open Access Journals (Sweden)

    Fontenille Didier

    2009-08-01

    Full Text Available Abstract Endemic malaria has been eradicated from France, but some falciparum malaria cases have been described in patients who have never travelled outside the country. Ms. V. 21 year-old and Mr. M. 23 year-old living together in Paris were on holiday in Saint Raphaël (French Riviera. They presented with fever, vertigo and nausea. A blood smear made to control thrombocytopaenia revealed intra-erythrocytic forms of Plasmodium falciparum. The parasitaemia level was 0.15% for Ms. V and 3.2% for Mr. M. This couple had no history of blood transfusion or intravenous drug use. They had never travelled outside metropolitan France, but had recently travelled around France: to Saint Mard (close to Paris Charles de Gaulle (CdG airport, to Barneville plage (in Normandy and finally to Saint Raphaël. The most probable hypothesis is an infection transmitted in Saint Mard by an imported anopheline mosquito at CdG airport. The DNA analysis of parasites from Ms. V.'s and Mr. M.'s blood revealed identical genotypes. Because it is unlikely that two different anopheline mosquitoes would be infected by exactly the same clones, the two infections must have been caused by the infective bites of the same infected mosquito.

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

    Energy Technology Data Exchange (ETDEWEB)

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

    2017-07-10

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

  18. Shocks and currents in stratified atmospheres with a magnetic null point

    Science.gov (United States)

    Tarr, Lucas A.; Linton, Mark

    2017-08-01

    We use the resistive MHD code LARE (Arber et al 2001) to inject a compressive MHD wavepacket into a stratified atmosphere that has a single magnetic null point, as recently described in Tarr et al 2017. The 2.5D simulation represents a slice through a small ephemeral region or area of plage. The strong gradients in field strength and connectivity related to the presence of the null produce substantially different dynamics compared to the more slowly varying fields typically used in simple sunspot models. The wave-null interaction produces a fast mode shock that collapses the null into a current sheet and generates a set of outward propagating (from the null) slow mode shocks confined to field lines near each separatrix. A combination of oscillatory reconnection and shock dissipation ultimately raise the plasma's internal energy at the null and along each separatrix by 25-50% above the background. The resulting pressure gradients must be balanced by Lorentz forces, so that the final state has contact discontinuities along each separatrix and a persistent current at the null. The simulation demonstrates that fast and slow mode waves localize currents to the topologically important locations of the field, just as their Alfvenic counterparts do, and also illustrates the necessity of treating waves and reconnection as coupled phenomena.

  19. Le développement touristique de deux sites chinois « incontournables » : Beihai et Guilin (Guangxi The tourist development of two « paramount » Chinese sites: Beihai and Guilin (Guangxi

    Directory of Open Access Journals (Sweden)

    Benjamin Taunay

    2008-12-01

    Full Text Available Le tourisme national dans la région autonome du Guangxi est fortement polarisé par la ville de Guilin, connue dans toute la Chine à cause de son site et de l’expression littéraire : « Le plus beau paysage est à Guilin ». L’analyse de la mise en tourisme de cette ville, ainsi que celle de Beihai - qualifiée de « plus belle plage sous le ciel » - montre des lieux aux structures et aux dynamiques spatiales singulières. L’analyse essaye également de souligner la croissance d’un tourisme de plus en plus individuel dans cette région.Domestic tourism in the Guangxi Autonomous Region stems mainly from the city of Guilin, known all over China because of its setting and because of the literary expression «the most beautiful landscape is in Guilin». The analysis of the tourist development of this city, as well as the city of Beihai – labelled  «most beautiful beach under the sky» – shows places with unique structures and spatial dynamics. The analysis also tries to underscore the growth of an increasingly individual type of tourism in the region.

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

    Energy Technology Data Exchange (ETDEWEB)

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

    2017-08-20

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

  1. Early evolution of an X-ray emitting solar active region

    International Nuclear Information System (INIS)

    Wolfson, C.J.; Acton, L.W.; Leibacher, J.W.; Roethig, D.T.

    1977-01-01

    The birth and early evolution of a solar active region has been investigated using X-ray observations from the Lockheed Mapping X-Ray Heliometer on board the OSO-8 spacecraft. X-ray emission is observed within three hours of the first detection of Hα plage. At that time, a plasma temperature of 4 x 10 6 K in a region having a density of the order of 10 10 cm -3 is inferred. During the fifty hours following birth almost continuous flares or flare-like X-ray bursts are superimposed on a monotonically increasing base level of X-ray emission produced by plasma with a temperature of the order 3 x 10 6 K. If it is assumed that the X-rays result from heating due to dissipation of current systems or magnetic field reconnection, it can be concluded that flare-like X-ray emission soon after active region birth implies that the magnetic field probably emerges in a stressed or complex configuration. (Auth.)

  2. Cine club

    CERN Multimedia

    Ciné club

    2010-01-01

    Monday 13 December 2010 at 18:30 / Lundi 13 Décembre 2010 à 18:30 CERN Main Auditorium / Amphithéâtre Principal Comme chaque année avant Noël, le CINE-CLUB du CERN est heureux d’inviter petits et grands à une projection gratuite du film.   Ponyo sur la falaise (Japon, 2008, Hayao Miyazaki) Le petit Sosuke vit avec sa mère sur une haute falaise surplombant la mer. Un beau jour, il découvre sur la plage caillouteuse Ponyo, une petite fille poisson. Ponyo est si fascinée par Sosuke et le monde terrestre que son désir le plus cher est de devenir un être humain. Mais Fujimoto, son magicien de père, n’est pas du tout d’accord avec cette idée et il la force à regagner les profondeurs de l’océan. Bien décidée à revoir Sosuke, Ponyo s’&...

  3. Origins of Solar Systems: Removing Activity-Related Radial Velocity Noise to Improve Extrasolar Planet Searches

    Science.gov (United States)

    Saar, Steven; Lindstrom, David (Technical Monitor)

    2003-01-01

    We have continued the super high resolution (R is approximately 200,000), high S/N (> 300) echelle study of joint line bisector and radial velocity variations using the McDonald 2-D coude. A long observing run in October 2002 was quite successful (8 clear nights). We now have close to three years of data, which begins to sample a good fraction of the magnetic cycle timescales for some of our targets (e.g., K Ceti; P(sub cyc)=5.6 yrs). This will be very helpful in unraveling the complex relationships between plage and v(sub r), changes which we have uncovered. A preliminary analysis of the limited data in hand, and find some tantalizing evidence for correlations between median line bisector displacement and radial velocity v(sub r). The correlation appears to be specific to the particular star being considered, probably since it is a function of both spectral type and rotation rate. Additional information regarding progress on the grant is included.

  4. Solar Cycle 24 UV Radiation: Lowest in more than 6 Decades

    Science.gov (United States)

    Schroder, Klaus-Peter; Mittag, Marco; Schmitt, J. H. M. M.

    2015-01-01

    Using spectra taken by the robotic telescope ``TIGRE'' (see Fig. 1 and the TIGRE-poster presented by Schmitt et al. at this conference) and its mid-resolution (R=20,000) HEROS double-channel echelle spectrograph, we present our measurements of the solar Ca II H&K chromospheric emission. Using moonlight, we applied the calibration and definition of the Mt. Wilson S-index , which allows a direct comparison with historic observations, reaching back to the early 1960's. At the same time, coming from the same EUV emitting plage regions, the Ca II H&K emission is a good proxy for the latter, which is of interest as a forcing factor in climate models. Our measurements probe the weak, asynchronous activity cycle 24 around its 2nd maximum during the past winter. Our S-values suggest that this maximum is the lowest in chromospheric emission since at least 60 years -- following the longest and deepest minimum since a century. Our observations suggest a similarly long-term (on a scale of decades) low of the far-UV radiation, which should be considered by the next generation of climate models. The current, very interesting activity behaviour calls for a concerted effort on long-term solar monitoring.

  5. TIME-DEPENDENT SUPPRESSION OF OSCILLATORY POWER IN EVOLVING SOLAR MAGNETIC FIELDS

    Energy Technology Data Exchange (ETDEWEB)

    Prasad, S. Krishna; Jess, D.B.; Keys, P.H. [Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, BT7 1NN (United Kingdom); Jain, R., E-mail: krishna.prasad@qub.ac.uk [School of Mathematics and Statistics, University of Sheffield, Sheffield S3 7RH (United Kingdom)

    2016-05-20

    Oscillation amplitudes are generally smaller within magnetically active regions like sunspots and plage when compared to their surroundings. Such magnetic features, when viewed in spatially resolved power maps, appear as regions of suppressed power due to reductions in the oscillation amplitudes. Employing high spatial- and temporal-resolution observations from the Dunn Solar Telescope (DST) in New Mexico, we study the power suppression in a region of evolving magnetic fields adjacent to a pore. By utilizing wavelet analysis, we study for the first time how the oscillatory properties in this region change as the magnetic field evolves with time. Image sequences taken in the blue continuum, G-band, Ca ii K, and H α filters were used in this study. It is observed that the suppression found in the chromosphere occupies a relatively larger area, confirming previous findings. Also, the suppression is extended to structures directly connected to the magnetic region, and is found to get enhanced as the magnetic field strength increased with time. The dependence of the suppression on the magnetic field strength is greater at longer periods and higher formation heights. Furthermore, the dominant periodicity in the chromosphere was found to be anti-correlated with increases in the magnetic field strength.

  6. Calculation of reactivity by digital processing; Calcul de la reactivite par traitement numerique

    Energy Technology Data Exchange (ETDEWEB)

    Hedde, J. [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1968-12-01

    With a view to exploring the new possibilities offered by digital techniques, a description is given of the optimum theoretical conditions of a computation of the realtime reactivity using counting samples (obtained from a nuclear reactor). The degree to which these optimum conditions can be attained depends on the complexity of the processing which can be accepted. A compromise thus has to be made between the accuracy required and the simplicity of the equipment carrying out the processing. An example is given, using a relatively simple structure, which gives an idea of the accuracy of the results obtained over a wide range of reactor power. (author) [French] Dans le but d'explorer les possibilites nouvelles des techniques numeriques, on decrit les conditions theoriques optimales d'un calcul de la reactivite en temps reel a partir d'echantillons de comptage (en provenance d'un reacteur nucleaire). Ces conditions optimales peuvent etre approchees d'autant mieux que l'on accepte un traitement plus complexe. Un compromis est donc a faire entre la precision desiree et la simplicite du materiel assurant le traitement. Un exemple adoptant une structure de complexite reduite permet de juger de la precision des resultats obtenus sur une importante plage d'evolution de la puissance. (auteur)

  7. NON-LTE INVERSIONS OF THE Mg ii h and k AND UV TRIPLET LINES

    Energy Technology Data Exchange (ETDEWEB)

    De la Cruz Rodríguez, Jaime; Leenaarts, Jorrit [Institute for Solar Physics, Dept. of Astronomy, Stockholm University, AlbaNova University Centre, SE-106 91 Stockholm Sweden (Sweden); Ramos, Andrés Asensio [Instituto de Astrofísica de Canarias, E-38205, La Laguna, Tenerife (Spain)

    2016-10-20

    The Mg ii h and k lines are powerful diagnostics for studying the solar chromosphere. They have become particularly popular with the launch of the Interface Region Imaging Spectrograph ( IRIS ) satellite, and a number of studies that include these lines have lead to great progress in understanding chromospheric heating, in many cases thanks to the support from 3D MHD simulations. In this study, we utilize another approach to analyze observations: non-LTE inversions of the Mg ii h and k and UV triplet lines including the effects of partial redistribution. Our inversion code attempts to construct a model atmosphere that is compatible with the observed spectra. We have assessed the capabilities and limitations of the inversions using the FALC atmosphere and a snapshot from a 3D radiation-MHD simulation. We find that Mg ii h and k allow reconstructing a model atmosphere from the middle photosphere to the transition region. We have also explored the capabilities of a multi-line/multi-atom setup, including the Mg ii h and k, the Ca ii 854.2 nm, and the Fe i 630.25 lines to recover the full stratification of physical parameters, including the magnetic field vector, from the photosphere to the chromosphere. Finally, we present the first inversions of observed IRIS spectra from quiet-Sun, plage, and sunspot, with very promising results.

  8. Chromospheric scaling laws, width-luminosity correlations, and the Wilson-Bappu effect

    International Nuclear Information System (INIS)

    Ayres, T.R.

    1979-01-01

    Simple scaling laws are developed to explain the thickness and mean electron density of late-type stellar chromospheres in an effort to understand why the emission cores of effectively thick resonance lines such as Ca II H and K broaden with increasing stellar luminosity (the Wilson-Bappu effect). It is shown that stellar chromospheres become thicker in mass column density as stellar gravity g decreases and that the mean chromospheric electric density n/sub e/ decreases if the chromospheric heating dF/dm is constant with height and if the total heating F/sup tot/ is independent of g. It is also shown that chromospheres becomes thicker and the mean electron density becomes larger than the total chromospheric heating increases. The predicted behavior of the K 1 minimum separation and full width at half-maximum of the Ca II emission core (W 0 ) based on the derived scaling laws agree quantitatively with the observed correlations of these widths with fundamental stellar parameters, particularly surface gravity. In addition, the predicted behavior of the K 2 peak separation and base emission width with increasing chromospheric heating is consistent with the behavior of the Ca II emission core shapes in solar plages. The analytical arguments suggest that the Wilson-Bappu effect is largely a consequence of hydrostatic equilibrium rather than chromospheric dynamics

  9. Recordings of solar protons during October 26-29, 1968

    International Nuclear Information System (INIS)

    Gjerde, A.; Amundsen, P.

    1974-08-01

    The composite events causing increased influx of solar particles during October 26-29, 1968 are studied using data from the polar orbiting ESRO IA satellite. Details on protons of 0.1-10 MeV are presented, and their interplanetary propagation characteristics discussed. Diffusion model fit to the prompt event commencing October 26, suggests an interplanetary diffusion coefficient for 200-350 keV protons of (2.8π+0.7).10 20 cm 2 s -1 . The most likely parent flare for this event is the 1N flare of 0119 UT October 26, occuring in McMath plage region 9740 at 32 deg E solar longitude. The slow decay of the event is then accounted for by co-rotation effects. The flares occurring in the same solar region on October 27 and leading to the delayed events of October 29, did not result in prompt events seen near the Earth, showing the great variability in energetic particle propagation conditions of interplanetary space. (auth)

  10. Calculation of reactivity by digital processing; Calcul de la reactivite par traitement numerique

    Energy Technology Data Exchange (ETDEWEB)

    Hedde, J [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1968-12-01

    With a view to exploring the new possibilities offered by digital techniques, a description is given of the optimum theoretical conditions of a computation of the realtime reactivity using counting samples (obtained from a nuclear reactor). The degree to which these optimum conditions can be attained depends on the complexity of the processing which can be accepted. A compromise thus has to be made between the accuracy required and the simplicity of the equipment carrying out the processing. An example is given, using a relatively simple structure, which gives an idea of the accuracy of the results obtained over a wide range of reactor power. (author) [French] Dans le but d'explorer les possibilites nouvelles des techniques numeriques, on decrit les conditions theoriques optimales d'un calcul de la reactivite en temps reel a partir d'echantillons de comptage (en provenance d'un reacteur nucleaire). Ces conditions optimales peuvent etre approchees d'autant mieux que l'on accepte un traitement plus complexe. Un compromis est donc a faire entre la precision desiree et la simplicite du materiel assurant le traitement. Un exemple adoptant une structure de complexite reduite permet de juger de la precision des resultats obtenus sur une importante plage d'evolution de la puissance. (auteur)

  11. Effect of stellar activity on the high precision transit light curve

    Directory of Open Access Journals (Sweden)

    Oshagh, M.

    2015-01-01

    Full Text Available Stellar activity features such as spots and plages can create difficulties in determining planetary parameters through spectroscopic and photometric observations. The overlap of a transiting planet and a stellar spot, for instance, can produce anomalies in the transit light curve that may lead to inaccurate estimation of the transit duration, depth, and timing. Such inaccuracies can affect the precise derivation of the planet’s radius. In this talk we will present the results of a quantitative study on the effects of stellar spots on high precision transit light curves. We show that spot anomalies can lead to the estimate of a planet radius that is 4% smaller than the real value. The effects on the transit duration can also be of the order of 4%, longer or shorter. Depending on the size and distribution of spots, anomalies can also produce transit timing variations with significant amplitudes. For instance, TTVs with signal amplitudes of 200 seconds can be produced by spots as large as the largest sunspot. Finally, we examine the impact of active regions on the transit depth measurements in different wavelengths, in order to probe the impact of this effect on transmission spectroscopy measurements. We show that significant (up to 10% underestimation/overestimation of the planet-to-star radius ratio can be measured, especially in the short wavelength regime.

  12. Initial phase of the development of sunspot groups and their forecast

    International Nuclear Information System (INIS)

    Berlyand, B.O.; Burov, V.A.; Stepanyan, N.N.

    1979-01-01

    Some characteristics of the initial phase of sunspot groups and their forecast have been considered. Experimental data on 340 sunspot groups were obtained in 1967-1969. It was found that oscillations of the magnetic flux in the groups indicate the possibility of the existence of typical periods (2 and 4 days) of the magnetic field development. Most of the groups appears in young plages. The probability of the protons injection from the young groups is very small. The typical time of the development of the proton centre is 10-30 days. The characteristics of the group on the first day of its existence are vaguely connected with the lifetime of the group. On the second and third days the magnetic characteristics (the summary magnetic flux and the number of the unipolar regions) have the highest correlation coefficient (approximately 70%) with the lifetime of the group. The problem of the group lifetime forecast was being solved with the pattern recognition technique. On the base of the second day observation of the existence of the group verification of the received forecast 14% exceeds the verification of the climatological forecast. The forecast of the Zurich class with the same technique is effective beginning with the fifth day of the group existence and the forecast of the flare activity of the group since the day of its appearance. The exceeding of the verification as compared with the climatological forecasts in these problems is 10% and 8% accordingly

  13. The relationship between solar activity and the H and K line cores in integrated sunlight

    International Nuclear Information System (INIS)

    Jebsen, D.E.; Mitchell, W.E. Jr.

    1978-01-01

    In this paper the authors present and analyze new data on the cores of the H and K lines of ionized calcium in the spectrum of integrated sunlight. The intensities of the components Hsub(2γ), H 3 , Hsub(2r), Ksub(2γ), K 3 , and Ksub(2r) in the line cores were measured in terms of the continuum intensity at 4000 A during a solar rotation in September 1969. Other data on these components, obtained at or close to the time of solar minimum (September 1964) and solar maximum (September 1968), were also included. The intensities of these features are compared with two indices of solar activity: the Ca II plage index and the 2800 MHZ signal. The average correlation coefficients between the intensities of the measured features and those indices were 0.69 and 0.64, respectively. The results are consistent with those of Bumba and Ruzickova-Topolova (1967) for a solar rotation period in 1965. The method and results should provide a detailed quantitative basis for the study of the activity cycles and rotation periods of solar-type stars. (Auth.)

  14. Ionizing radiation control of Tribolium castaneum in wheat flour type 000

    International Nuclear Information System (INIS)

    Ritacco, M.

    1988-01-01

    The insects, mainly those of the coleoptera order, produce serious changes on the grains and flours, producing in some regions up to 50 % loss. Taking in account the information available up to date, this experiment consists of putting under the effect of the ionizing radiation specimens of Tribolium castaneum feeded with bread flour type 000, with the purpose of controling their biological cycle. They received gamma radiation doses between 250 and 2000 Gy, using 60 Co source. The daily observation made over a population of 590 insects, indicates the efficiency of the procedure, non toxic, which provokes the sterility at 250 Gy and inmediate dead starting at 1750 Gy. On the other hand, it was verified that the DL 50 on the insects irradiated at the lower of eight different doses applied, reaches 15,3 days, against the 162,6 days of the reference Tribolium. Then it is concluded that it is technologically feasible the application of ionizing radiation to the bread wheat flour type 000 for controling this main plage. (Author) [es

  15. Urbanisation côtière en Algérie, Processus et impacts sur l’environnement : Le cas de la baie d’Aïn el Turck Coastal urbanization in Algeria, Processes and Environment Impacts : The case of the Bay Aïn el Turck

    Directory of Open Access Journals (Sweden)

    Ghodbani Tarik

    2012-04-01

    Full Text Available A quelques kilomètres d’Oran, la zone côtière d’Aïn el Turck connue auparavant pour ses belles plages, a subi depuis quelques décennies une urbanisation incontrôlée touchant essentiellement son domaine public maritime (DPM. Actuellement, sur les parties hautes des plages comme Saint Roch, Paradis, Bouisseville ou Trouville s’alignent des villas de un à deux étages, des garages à bateaux et de grands hôtels. L’empiètement sur ces espaces pourtant protégés par plusieurs lois, a participé à l’érosion de la bande sableuse et à la régression de l’activité touristique balnéaire. Une situation qui reflète une nette difficulté dans la gestion et la protection de cet espace convoité et fragile.Notre étude de la zone côtière d’Aïn el Turck va aborder quatre points : la relation entre la « bétonisation » du rivage et le changement du trait de côte, l’évolution de l’urbanisation et les stratégies d’occupations, les types de concurrence qui existent entre différents usagers sur l’appropriation du foncier littoral et enfin, les difficultés éprouvées dans la protection du domaine public maritime par les services gestionnaires. La méthode du travail est basée essentiellement sur deux approches : la première est la comparaison entre plusieurs photos aériennes, à différentes dates, pour l’identification des changements naturels affectant le rivage en relation avec l’évolution de l’urbanisation de la côte. La seconde est la réalisation d’entretiens avec les principaux acteurs du territoire et l’analyse des discours formulés par les différents groupes d’intérêts, souvent en situation de conflit.A few kilometres from Oran, the coastal area of Ain el Turck previously known for its beautiful beaches, has suffered in recent decades uncontrolled urbanization affecting mainly the maritime public domain (DPM. Currently, the upper parts of beaches like St. Roch, Paradis, Trouville

  16. Impactos ambientais decorrentes da ocupação de áreas reguladoras do aporte de areia: a planície Costeira da Caponga, município de Cascavel, litoral leste cearense.

    Directory of Open Access Journals (Sweden)

    Antonio Jeovah de Andrade Meireles

    2008-03-01

    Full Text Available Pour définir les impacts environnementaux associés à l'occupation humaine dans des secteurs caractérisés par l'apport de sédiments (bypass sur la plage, via des champ de dunes et l’estuaire, ont été réalisées des études géo-environnementales dans la plaine côtière du Caponga, en y incluant un promontoire, une bande littorale et l’embouchure du canal estuarien de même nom. Les résultats ont été représentés dans des modèles évolutifs, intégrés à partir de la définition des flux de matière et d'énergie qui transitent dans la zone côtière. Les conséquences de l'expansion urbaine sur le promontoire, les dunes, la plage et le canal estuarien ont été caractérisées afin de définir des mesures adaptées de planification et de gestion.Environmental impacts caused by the occupation of areas regulating the sand input to the coast line in the coastal plain of Caponga, Cascavel town, East Coast of Ceará. To determine the environmental impacts related to human occupation in areas characterized by the input of sediments (bypass to the coastal line, through dunes and estuary, we carried out geoenvironmental studies in the coastal plain of Caponga. They included sections represented by a headland, coastal line and river mouth of the estuarine channel of Caponga. The results were represented in integrated evolutionary models based on the definition of flows of matter and energy that occur in the coastal area. The effects of urban expansion on the headland, dunes, shore and estuarine channel were characterized so as to define adequate measures of planning and management.Para definir os impactos ambientais associados à ocupação humana em áreas caracterizadas pelo aporte de sedimentos (bypass para a faixa de praia, via campo de dunas e estuário, foram realizados estudos geoambientais na planície costeira da Caponga, abrangendo setores representados por um promontório, faixa litorânea e desembocadura do canal estuarino

  17. Microwave emission from the coronae of late-type dwarf stars

    Energy Technology Data Exchange (ETDEWEB)

    Linsky, J.L.; Gary, D.E.

    1983-11-15

    We present VLA microwave observatios of 14 late-type dwarf and subgiant stars ad binary systems. In this extensive set of observations we detected four sources at 6 cm (chi/sup 1/ Ori, UV Cet, YY Gem, and Wolf 630AB) and found low upper limits for the remaining stars. The microwave luminosities of the nondetected F--K dwarfs are as small as 10/sup -2/ those of the dMe stars. The detected emission is slowly variable in all cases and is consistent with gyroresonant emission from thermal electrons spiralig in magnetic fields of about 300 gauss if the source sizes are as large as R/R/sub asterisk/roughly-equal3--4. This would correspond to magnetic fields that are probably in the range 10/sup 3/--10/sup 4/ gauss at the photospheric level. These photospheric field strengths are somewhat larger than have been observed so far in G--K dwarfs. An alternative mechanism is gyrosynchrotron emission from a relatively small number of electrons (only 10/sup -3/ the number of ambient electrons) with effective temperature, T/sub eff/>10/sup 8/ K. This mechanism is consistent with much smaller and presumably more realistic source sizes. Observations of YY gem dMle+dMle) at a number of phase are consistent with maximum but variable microwave flux at the same phase as miximum plage and central meridian passage of a large starspot of the secondary star. If confirmed by subsequent observations, this provides the first direct evidence that the emission process is magnetic in character on dMe stars.

  18. Influence of the Atmospheric Model on Hanle Diagnostics

    Science.gov (United States)

    Ishikawa, Ryohko; Uitenbroek, Han; Goto, Motoshi; Iida, Yusuke; Tsuneta, Saku

    2018-05-01

    We clarify the uncertainty in the inferred magnetic field vector via the Hanle diagnostics of the hydrogen Lyman-α line when the stratification of the underlying atmosphere is unknown. We calculate the anisotropy of the radiation field with plane-parallel semi-empirical models under the nonlocal thermal equilibrium condition and derive linear polarization signals for all possible parameters of magnetic field vectors based on an analytical solution of the atomic polarization and Hanle effect. We find that the semi-empirical models of the inter-network region (FAL-A) and network region (FAL-F) show similar degrees of anisotropy in the radiation field, and this similarity results in an acceptable inversion error ( e.g., {˜} 40 G instead of 50 G in field strength and {˜} 100° instead of 90° in inclination) when FAL-A and FAL-F are swapped. However, the semi-empirical models of FAL-C (averaged quiet-Sun model including both inter-network and network regions) and FAL-P (plage regions) yield an atomic polarization that deviates from all other models, which makes it difficult to precisely determine the magnetic field vector if the correct atmospheric model is not known ( e.g., the inversion error is much larger than 40% of the field strength; {>} 70 G instead of 50 G). These results clearly demonstrate that the choice of model atmosphere is important for Hanle diagnostics. As is well known, one way to constrain the average atmospheric stratification is to measure the center-to-limb variation of the linear polarization signals. The dependence of the center-to-limb variations on the atmospheric model is also presented in this paper.

  19. Staring Contests in the Overlord Embroidery Jeux de regards dans la Tapisserie du Débarquement

    Directory of Open Access Journals (Sweden)

    Nicole Terrien

    2012-03-01

    Full Text Available Appelée broderie en anglais, la Tapisserie du Débarquement offre une représentation originale de la Seconde Guerre mondiale susceptible d’attirer un public plus large que celui qui s’intéresse aux peintures traditionnelles ou aux récits de guerre. Inspirée de la Tapisserie de Bayeux, officiellement considérée comme un manuscrit, cette broderie peut et doit être lue comme un texte. Si nous la soumettons au même type d’explication de texte qu’un récit en mots, nous constatons que l’impression d’ensemble repose sur une série de détails qui confèrent une grande humanité à la représentation globale. En nous focalisant sur la représentation des yeux, nous pouvons retracer une évolution qui dépasse la simple évolution chronologique. Dès que les yeux deviennent visibles, les personnages gagnent une individualité. Les ennemis deviennent humains, partagent les mêmes émotions que les héros qui se battent pour la liberté. La mort se lit dans les regards vacants des corps gisant sur les plages ou le long des routes. Croisant le regard des personnages brodés, le spectateur est invité à balayer la tapisserie du regard, suivant des lignes moins évidentes que celles de la lecture horizontale. Le spectateur se trouve alors au cœur de l’action, partageant des émotions complexes. La nécessité constante de reconstruire le schéma transforme ce qui aurait pu être un outil de propagande en véritable œuvre d’art originale.

  20. Diagnostics of vector magnetic fields

    Science.gov (United States)

    Stenflo, J. O.

    1985-01-01

    It is shown that the vector magnetic fields derived from observations with a filter magnetograph will be severely distorted if the spatially unresolved magnetic structure is not properly accounted for. Thus the apparent vector field will appear much more horizontal than it really is, but this distortion is strongly dependent on the area factor and the temperature line weakenings. As the available fluxtube models are not sufficiently well determined, it is not possible to correct the filter magnetograph observations for these effects in a reliable way, although a crude correction is of course much better than no correction at all. The solution to this diagnostic problem is to observe simultaneously in suitable combinations of spectral lines, and/or use Stokes line profiles recorded with very high spectral resolution. The diagnostic power of using a Fourier transform spectrometer for polarimetry is shown and some results from I and V spectra are illustrated. The line asymmetries caused by mass motions inside the fluxtubes adds an extra complication to the diagnostic problem, in particular as there are indications that the motions are nonstationary in nature. The temperature structure appears to be a function of fluxtube diameter, as a clear difference between plage and network fluxtubes was revealed. The divergence of the magnetic field with height plays an essential role in the explanation of the Stokes V asymmetries (in combination with the mass motions). A self consistent treatment of the subarcsec field geometry may be required to allow an accurate derivation of the spatially averaged vector magnetic field from spectrally resolved data.

  1. Observing the Sun with the Atacama Large Millimeter/submillimeter Array (ALMA): Fast-Scan Single-Dish Mapping

    Science.gov (United States)

    White, S. M.; Iwai, K.; Phillips, N. M.; Hills, R. E.; Hirota, A.; Yagoubov, P.; Siringo, G.; Shimojo, M.; Bastian, T. S.; Hales, A. S.; Sawada, T.; Asayama, S.; Sugimoto, M.; Marson, R. G.; Kawasaki, W.; Muller, E.; Nakazato, T.; Sugimoto, K.; Brajša, R.; Skokić, I.; Bárta, M.; Kim, S.; Remijan, A. J.; de Gregorio, I.; Corder, S. A.; Hudson, H. S.; Loukitcheva, M.; Chen, B.; De Pontieu, B.; Fleishmann, G. D.; Gary, D. E.; Kobelski, A.; Wedemeyer, S.; Yan, Y.

    2017-07-01

    The Atacama Large Millimeter/submillimeter Array (ALMA) radio telescope has commenced science observations of the Sun starting in late 2016. Since the Sun is much larger than the field of view of individual ALMA dishes, the ALMA interferometer is unable to measure the background level of solar emission when observing the solar disk. The absolute temperature scale is a critical measurement for much of ALMA solar science, including the understanding of energy transfer through the solar atmosphere, the properties of prominences, and the study of shock heating in the chromosphere. In order to provide an absolute temperature scale, ALMA solar observing will take advantage of the remarkable fast-scanning capabilities of the ALMA 12 m dishes to make single-dish maps of the full Sun. This article reports on the results of an extensive commissioning effort to optimize the mapping procedure, and it describes the nature of the resulting data. Amplitude calibration is discussed in detail: a path that uses the two loads in the ALMA calibration system as well as sky measurements is described and applied to commissioning data. Inspection of a large number of single-dish datasets shows significant variation in the resulting temperatures, and based on the temperature distributions, we derive quiet-Sun values at disk center of 7300 K at λ = 3 mm and 5900 K at λ = 1.3 mm. These values have statistical uncertainties of about 100 K, but systematic uncertainties in the temperature scale that may be significantly larger. Example images are presented from two periods with very different levels of solar activity. At a resolution of about 25'', the 1.3 mm wavelength images show temperatures on the disk that vary over about a 2000 K range. Active regions and plages are among the hotter features, while a large sunspot umbra shows up as a depression, and filament channels are relatively cool. Prominences above the solar limb are a common feature of the single-dish images.

  2. CHROMOSPHERIC SIGNATURES OF SMALL-SCALE FLUX EMERGENCE AS OBSERVED WITH NEW SOLAR TELESCOPE AND HINODE INSTRUMENTS

    International Nuclear Information System (INIS)

    Yurchyshyn, V. B.; Goode, P. R.; Abramenko, V. I.; Chae, J.; Cao, W.; Andic, A.; Ahn, K.

    2010-01-01

    With the ever-increasing influx of high-resolution images of the solar surface obtained at a multitude of wavelengths, various processes occurring at small spatial scales have become a greater focus of our attention. Complex small-scale magnetic fields have been reported that appear to have enough stored energy to heat the chromosphere. While significant progress has been made in understanding small-scale phenomena, many specifics remain elusive. We present here a detailed study of a single event of disappearance of a magnetic dipole and associated chromospheric activity. Based on New Solar Telescope Hα data and Hinode photospheric line-of-sight magnetograms and Ca II H images, we report the following. (1) Our analysis indicates that even very small dipoles (elements separated by about 0.''5 or less) may reach the chromosphere and trigger non-negligible chromospheric activity. (2) Careful consideration of the magnetic environment where the new flux is deposited may shed light on the details of magnetic flux removal from the solar surface. We argue that the apparent collision and disappearance of two opposite polarity elements may not necessarily indicate their cancellation (i.e., reconnection, emergence of a 'U' tube, or submergence of Ω loops). In our case, the magnetic dipole disappeared by reconnecting with overlying large-scale inclined plage fields. (3) Bright points (BPs) seen in off-band Hα images are very well correlated with the Ca II H BPs, which in turn are cospatial with G-band BPs. We further speculate that, in general, Hα BPs are expected to be cospatial with photospheric BPs; however, a direct comparison is needed to refine their relationship.

  3. August 1972 solar-terrestrial events: interplanetary magnetic field observations

    Energy Technology Data Exchange (ETDEWEB)

    Smith, E J [Jet Propulsion Lab., Pasadena, Calif. (USA)

    1976-10-01

    A review is presented of the interplanetary magnetic field observations acquired in early August 1972 when four solar flares erupted in McMath Plage region 1976. Measurements of the interplanetary field were obtained by Earth satellites, HEOS-2 and Explorer 41, and by Pioneers 9 and 10 which, by good fortune, were radially aligned and only 45/sup 0/ east of the Earth-Sun direction. In response to the four flares, four interplanetary shocks were seen at Earth and at Pioneer 9, which was then at a heliocentric distance of 0.78 AU. However, at Pioneer 10, which was 2.2 AU from the Sun, only two forward shocks and one reverse shock were seen. The available magnetic field data acquired in the vicinity of the shocks are presented. Efforts to identify corresponding shocks at the several locations and to deduce their velocities of propagation between 0.8 and 2.2 AU are reviewed. The early studies were based on average velocities between the Sun and Pioneer 9, the Sun and Earth and the Sun and Pioneer 10. A large deceleration of the shocks between the Sun and 0.8 AU as well as between 0.8 and 2.2 AU was inferred. More recently the local velocities of the shocks at Pioneers 9 and 10 have become available. A comparision of these velocities shows little, if any, deceleration between 0.8 and 2.2 AU and implies that most or all of the deceleration actually occurred nearer the Sun. Evidence is also presented that shows a significant departure of the flare-generated shock fronts from spherical symmetry.

  4. Temporal and Latitudinal Variations of the Length-Scales and Relative Intensities of the Chromospheric Network

    Science.gov (United States)

    Raju, K. P.

    2018-05-01

    The Calcium K spectroheliograms of the Sun from Kodaikanal have a data span of about 100 years and covers over 9 solar cycles. The Ca line is a strong chromospheric line dominated by chromospheric network and plages which are good indicators of solar activity. Length-scales and relative intensities of the chromospheric network have been obtained in the solar latitudes from 50 degree N to 50 degree S from the spectroheliograms. The length-scale was obtained from the half-width of the two-dimensional autocorrelation of the latitude strip which gives a measure of the width of the network boundary. As reported earlier for the transition region extreme ultraviolet (EUV) network, relative intensity and width of the chromospheric network boundary are found to be dependent on the solar cycle. A varying phase difference has been noticed in the quantities in different solar latitudes. A cross-correlation analysis of the quantities from other latitudes with ±30 degree latitude revealed an interesting phase difference pattern indicating flux transfer. Evidence of equatorward flux transfer has been observed. The average equatorward flux transfer was estimated to be 5.8 ms-1. The possible reasons of the drift could be meridional circulation, torsional oscillations, or the bright point migration. Cross-correlation of intensity and length-scale from the same latitude showed increasing phase difference with increasing latitude. We have also obtained the cross correlation of the quantities across the equator to see the possible phase lags in the two hemispheres. Signatures of lags are seen in the length scales of southern hemisphere near the equatorial latitudes, but no such lags in the intensity are observed. The results have important implications on the flux transfer over the solar surface and hence on the solar activity and dynamo.

  5. Propagating Disturbances in Coronal Loops: A Detailed Analysis of Propagation Speeds

    Science.gov (United States)

    Kiddie, G.; De Moortel, I.; Del Zanna, G.; McIntosh, S. W.; Whittaker, I.

    2012-08-01

    Quasi-periodic disturbances have been observed in the outer solar atmosphere for many years. Although first interpreted as upflows (Schrijver et al., Solar Phys. 187, 261, 1999), they have been widely regarded as slow magneto-acoustic waves, due to their observed velocities and periods. However, recent observations have questioned this interpretation, as periodic disturbances in Doppler velocity, line width, and profile asymmetry were found to be in phase with the intensity oscillations (De Pontieu and McIntosh, Astrophys. J. 722, 1013, 2010; Tian, McIntosh, and De Pontieu, Astrophys. J. Lett. 727, L37, 2011), suggesting that the disturbances could be quasi-periodic upflows. Here we conduct a detailed analysis of the velocities of these disturbances across several wavelengths using the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). We analysed 41 examples, including both sunspot and non-sunspot regions of the Sun. We found that the velocities of propagating disturbances (PDs) located at sunspots are more likely to be temperature dependent, whereas the velocities of PDs at non-sunspot locations do not show a clear temperature dependence. This suggests an interpretation in terms of slow magneto-acoustic waves in sunspots but the nature of PDs in non-sunspot (plage) regions remains unclear. We also considered on what scale the underlying driver is affecting the properties of the PDs. Finally, we found that removing the contribution due to the cooler ions in the 193 Å wavelength suggests that a substantial part of the 193 Å emission of sunspot PDs can be attributed to the cool component of 193 Å.

  6. An absolute nuclear magnetic resonance magnetometer; Magnetometre absolu a resonance magnetique nucleaire

    Energy Technology Data Exchange (ETDEWEB)

    Salvi, A [Commisariat a l' Energie Atomique, Grenoble (France). Centre d' Etudes Nucleaires

    1961-10-15

    After an introduction in which the various work undertaken since the discovery of nuclear magnetic resonance is rapidly reviewed, the author describes briefly In the first chapter three types of NMR magnetometers, giving the advantages and disadvantages of each of them and deducing from this the design of the apparatus having the greatest number of qualities Chapter II is devoted to the crossed coil nuclear oscillator which operates continuously over a wide range (800 gamma). To avoid an error due to a carrying over the frequency, the measurement is carried out using bands of 1000 {gamma}. Chapter III deals with frequency measurements. The author describes an original arrangement which makes possible the frequency-field conversion with an accuracy of {+-} 5 x 10{sup -6}, and the differential measurement between two nuclear oscillators. The report finishes with a conclusion and a few recordings. (author) [French] Apres une introduction rappelant les divers travaux effectues en resonance magnetique nucleaire depuis sa mise en evidence, l'auteur decrit sommairement dans le premier chapitre trois types de magnetometre a R.M.N. enumerant les avantages et les inconvenients de chacun a partir desquels il projet, l'appareillage reunissant le maximum de qualites. Le chapitre II est consacre a l'oscillateur nucleaire a bobines croisees permettant un fonctionnement continu dons une large plage (800 gamma). Pour eviter une erreur due a l'entrainement de frequence, la mesure s'effectue par bandes de 1000 {gamma} chacune. Le chapitre III traite la mesure de frequence. L'auteur expose un montage original permettant la traduction frequence-champ avec une precision egale a {+-} 5.10{sup -6}, et la mesure differentielle entre deux oscillateurs nucleaires. Une conclusion et quelques enregistrements terminent ce travail. (auteur)

  7. Midterm Periodicity Analysis of the Mount Wilson Magnetic Indices Using the Synchrosqueezing Transform

    Energy Technology Data Exchange (ETDEWEB)

    Feng, Song; Wang, Feng; Deng, Hui; Yang, Yunfei [Yunnan Key Laboratory of Computer Technology Application/Faculty of Information Engineering and Automation, Kunming University of Science and Technology, Kunming 650500 (China); Yu, Lan, E-mail: ynkmfs@escience.cn [Department of Mechanical and Electrical Engineering, Yunnan Land and Resources Vocational College, Kunming 650217 (China)

    2017-08-10

    A novel time–frequency technique, called the synchrosqueezing transform (SST), is used to investigate the midterm periodic variations of magnetic fields on the solar surface. The Magnetic Plage Strength Index (MPSI) and the Mount Wilson Sunspot Index (MWSI), measured daily by the Mount Wilson Observatory between 1970 January 19 and 2012 January 22, are selected. Short-, mid, and longer-term periodicities are represented and decomposed by the SST with hardly any mode mixing. This demonstrates that the SST is a useful time–frequency analysis technique to characterize the periodic modes of helioseismic data. Apart from the fundamental modes of the annual periodicity, ∼27 day rotational cycle and ∼11 year solar cycle, the SST reveals several midterm periodicities in the two magnetic activity indices, specifically, ∼157 days (i.e., Rieger-type periodicity), and ∼1.3 and 1.7 years. The periodic modes, with 116.4 and 276.2 day periodicity in the MPSI, 108.5 and 251.6 day periodicity in the MWSI, and 157.7 day periodicity in the two indices, are in better accord with those significant periodicities derived from the Rossby waves theoretical model. This study suggests that the modes are caused by Rossby waves. For the 1.30 and 1.71 year periodicity of the MPSI, and the 1.33 and 1.67 year periodicity of the MWSI, our analysis infers that they are related to those periodicities with the same timescale in the interior of the Sun and in the high atmospheric layers.

  8. Observations of photospheric magnetic fields and shear flows in flaring active regions

    International Nuclear Information System (INIS)

    Tarbell, T.; Ferguson, S.; Frank, Z.; Title, A.; Topka, K.

    1988-01-01

    Horizontal flows in the photosphere and subsurface convection zone move the footpoints of coronal magnetic field lines. Magnetic energy to power flares can be stored in the corona if the flows drive the fields far from the potential configuration. Videodisk movies were shown with 0.5 to 1 arcsecond resolution of the following simultaneous observations: green continuum, longitudinal magnetogram, Fe I 5576 A line center (mid-photosphere), H alpha wings, and H alpha line center. The movies show a 90 x 90 arcsecond field of view of an active region at S29, W11. When viewed at speeds of a few thousand times real-time, the photospheric movies clearly show the active region fields being distorted by a remarkable combination of systematic flows and small eruptions of new flux. Magnetic bipoles are emerging over a large area, and the polarities are systematically flowing apart. The horizontal flows were mapped in detail from the continuum movies, and these may be used to predict the future evolution of the region. The horizontal flows are not discernable in H alpha. The H alpha movies strongly suggest reconnection processes in the fibrils joining opposite polarities. When viewed in combination with the magnetic movies, the cause for this evolution is apparent: opposite polarity fields collide and partially cancel, and the fibrils reconnect above the surface. This type of reconnection, driven by subphotospheric flows, complicates the chromospheric and coronal fields, causing visible braiding and twisting of the fibrils. Some of the transient emission events in the fibrils and adjacent plage may also be related

  9. A Decade of H α Transits for HD 189733 b: Stellar Activity versus Absorption in the Extended Atmosphere

    Energy Technology Data Exchange (ETDEWEB)

    Cauley, P. Wilson; Redfield, Seth [Wesleyan University, Astronomy Department, Van Vleck Observatory, 96 Foss Hill Drive, Middletown, CT 06459 (United States); Jensen, Adam G., E-mail: pcauley@wesleyan.edu [University of Nebraska-Kearney, Department of Physics and Astronomy, 24011 11th Avenue, Kearney, NE 68849 (United States)

    2017-05-01

    HD 189733 b is one of the most well studied exoplanets due to its large transit depth and host star brightness. The focus on this object has produced a number of high-cadence transit observations using high-resolution optical spectrographs. Here we present an analysis of seven full H α transits of HD 189733 b using HARPS on the 3.6 meter La Silla telescope and HIRES on Keck I, taken over the course of nine years from 2006 to 2015. H α transmission signals are analyzed as a function of the stellar activity level, as measured using the normalized core flux of the Ca ii H and K lines. We find strong variations in the strength of the H α transmission spectrum from epoch to epoch. However, there is no clear trend between the Ca ii core emission and the strength of the in-transit H α signal, although the transit showing the largest absorption value also occurs when the star is the most active. We present simulations of the in-transit contrast effect and find that the planet must consistently transit active latitudes with very strong facular and plage emission regions in order to reproduce the observed line strengths. We also investigate the measured velocity centroids with models of planetary rotation and show that the small line profile velocities could be due to large velocities in the upper atmosphere of the planet. Overall, we find it more likely that the measured H α signals arise in the extended planetary atmosphere, although a better understanding of active region emission for active stars such as HD 189733 is needed.

  10. Exoplanet Transits of Stellar Active Regions

    Science.gov (United States)

    Giampapa, Mark S.; Andretta, Vincenzo; Covino, Elvira; Reiners, Ansgar; Esposito, Massimiliano

    2018-01-01

    We report preliminary results of a program to obtain high spectral- and temporal-resolution observations of the neutral helium triplet line at 1083.0 nm in transiting exoplanet systems. The principal objective of our program is to gain insight on the properties of active regions, analogous to solar plages, on late-type dwarfs by essentially using exoplanet transits as high spatial resolution probes of the stellar surface within the transit chord. The 1083 nm helium line is a particularly appropriate diagnostic of magnetized areas since it is weak in the quiet photosphere of solar-type stars but appears strongly in absorption in active regions. Therefore, during an exoplanet transit over the stellar surface, variations in its absorption equivalent width can arise that are functions of the intrinsic strength of the feature in the active region and the known relative size of the exoplanet. We utilized the Galileo Telescope and the GIANO-B near-IR echelle spectrograph to obtain 1083 nm spectra during transits in bright, well-known systems that include HD 189733, HD 209458, and HD 147506 (HAT-P-2). We also obtained simultaneous auxiliary data on the same telescope with the HARPS-N UV-Visible echelle spectrograph. We will present preliminary results from our analysis of the observed variability of the strength of the He I 1083 nm line during transits.Acknowledgements: Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The NSO is operated by AURA under a cooperative agreement with the NSF.

  11. A comparison study of a solar active-region eruptive filament and a neighboring non-eruptive filament

    Science.gov (United States)

    Jiang, Chao-Wei; Wu, Shi-Tsan; Feng, Xue-Shang; Hu, Qiang

    2016-01-01

    Solar active region (AR) 11283 is a very magnetically complex region and it has produced many eruptions. However, there exists a non-eruptive filament in the plage region just next to an eruptive one in the AR, which gives us an opportunity to perform a comparison analysis of these two filaments. The coronal magnetic field extrapolated using our CESE-MHD-NLFFF code reveals that two magnetic flux ropes (MFRs) exist in the same extrapolation box supporting these two filaments, respectively. Analysis of the magnetic field shows that the eruptive MFR contains a bald-patch separatrix surface (BPSS) cospatial very well with a pre-eruptive EUV sigmoid, which is consistent with the BPSS model for coronal sigmoids. The magnetic dips of the non-eruptive MFRs match Hα observation of the non-eruptive filament strikingly well, which strongly supports the MFR-dip model for filaments. Compared with the non-eruptive MFR/filament (with a length of about 200 Mm), the eruptive MFR/filament is much smaller (with a length of about 20 Mm), but it contains most of the magnetic free energy in the extrapolation box and holds a much higher free energy density than the non-eruptive one. Both the MFRs are weakly twisted and cannot trigger kink instability. The AR eruptive MFR is unstable because its axis reaches above a critical height for torus instability, at which the overlying closed arcades can no longer confine the MFR stably. On the contrary, the quiescent MFR is very firmly held by its overlying field, as its axis apex is far below the torus-instability threshold height. Overall, this comparison investigation supports that an MFR can exist prior to eruption and the ideal MHD instability can trigger an MFR eruption.

  12. A comparison study of a solar active-region eruptive filament and a neighboring non-eruptive filament

    International Nuclear Information System (INIS)

    Jiang, Chao-Wei; Feng, Xue-Shang; Wu, Shi-Tsan; Hu, Qiang

    2016-01-01

    Solar active region (AR) 11283 is a very magnetically complex region and it has produced many eruptions. However, there exists a non-eruptive filament in the plage region just next to an eruptive one in the AR, which gives us an opportunity to perform a comparison analysis of these two filaments. The coronal magnetic field extrapolated using our CESE–MHD–NLFFF code reveals that two magnetic flux ropes (MFRs) exist in the same extrapolation box supporting these two filaments, respectively. Analysis of the magnetic field shows that the eruptive MFR contains a bald-patch separatrix surface (BPSS) cospatial very well with a pre-eruptive EUV sigmoid, which is consistent with the BPSS model for coronal sigmoids. The magnetic dips of the non-eruptive MFRs match Hα observation of the non-eruptive filament strikingly well, which strongly supports the MFR-dip model for filaments. Compared with the non-eruptive MFR/filament (with a length of about 200 Mm), the eruptive MFR/filament is much smaller (with a length of about 20 Mm), but it contains most of the magnetic free energy in the extrapolation box and holds a much higher free energy density than the non-eruptive one. Both the MFRs are weakly twisted and cannot trigger kink instability. The AR eruptive MFR is unstable because its axis reaches above a critical height for torus instability, at which the overlying closed arcades can no longer confine the MFR stably. On the contrary, the quiescent MFR is very firmly held by its overlying field, as its axis apex is far below the torus-instability threshold height. Overall, this comparison investigation supports that an MFR can exist prior to eruption and the ideal MHD instability can trigger an MFR eruption. (paper)

  13. EarthFinder: A Precise Radial Velocity Survey Probe Mission of our Nearest Stellar Neighbors for Earth-Mass Habitable Zone Analogs Using High-Resolution UV-Vis-NIR Echelle Spectroscopy on a Space Platform

    Science.gov (United States)

    Plavchan, Peter; EarthFinder Team

    2018-01-01

    We are investigating the science case for a 1.0-1.4 meter space telescope to survey the closest, brightest FGKM main sequence stars to search for Habitable Zone (HZ) Earth analogs using the precise radial velocity (PRV) technique at a precision of 1-10 cm/s. Our baseline instrument concept uses two diffraction-limited spectrographs operating in the 0.4-1.0 microns and 1.0-2.4 microns spectral regions each with a spectral resolution of R=150,000~200,000, with the possibility of a third UV arm. Because the instrument utilizes a diffraction-limited input beam, the spectrograph would be extremely compact, less than 50 cm on a side, and illumination can be stabilized with the coupling of starlight into single mode fibers. With two octaves of wavelength coverage and a cadence unimpeded by any diurnal, seasonal, and atmospheric effects, EarthFinder will offer a unique platform for recovering stellar activity signals from starspots, plages, granulation, etc. to detect exoplanets at velocity semi-amplitudes currently not obtainable from the ground. Variable telluric absorption and emission lines may potentially preclude achieving PRV measurements at or below 10 cm/s in the visible and advantage compared to an annual ~3-6 month observing season from the ground for mitigating stellar activity and detecting the orbital periods of HZ Earth-mass analogs (e.g. ~6-months to ~2 years). Finally, we are compiling a list of ancillary science cases for the observatory, ranging from asteroseismology to the direct measurement of the expansion of the Universe.

  14. An HST/STIS Optical Transmission Spectrum of Warm Neptune GJ 436b

    Science.gov (United States)

    Lothringer, Joshua D.; Benneke, Björn; Crossfield, Ian J. M.; Henry, Gregory W.; Morley, Caroline; Dragomir, Diana; Barman, Travis; Knutson, Heather; Kempton, Eliza; Fortney, Jonathan; McCullough, Peter; Howard, Andrew W.

    2018-02-01

    GJ 436b is a prime target for understanding warm Neptune exoplanet atmospheres and a target for multiple James Webb Space Telescope (JWST) Guaranteed Time Observation programs. Here, we report the first space-based optical transmission spectrum of the planet using two Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) transit observations from 0.53 to 1.03 μm. We find no evidence for alkali absorption features, nor evidence of a scattering slope longward of 0.53 μm. The spectrum is indicative of moderate to high metallicity (∼100–1000× solar), while moderate-metallicity scenarios (∼100× solar) require aerosol opacity. The optical spectrum also rules out some highly scattering haze models. We find an increase in transit depth around 0.8 μm in the transmission spectra of three different sub-Jovian exoplanets (GJ 436b, HAT-P-26b, and GJ 1214b). While most of the data come from STIS, data from three other instruments may indicate this is not an instrumental effect. Only the transit spectrum of GJ 1214b is well fit by a model with stellar plages on the photosphere of the host star. Our photometric monitoring of the host star reveals a stellar rotation rate of 44.1 days and an activity cycle of 7.4 years. Intriguingly, GJ 436 does not become redder as it gets dimmer, which is expected if star spots were dominating the variability. These insights into the nature of the GJ 436 system help refine our expectations for future observations in the era of JWST, whose higher precision and broader wavelength coverage will shed light on the composition and structure of GJ 436b’s atmosphere.

  15. A hybrid system for solar irradiance specification

    Science.gov (United States)

    Tobiska, W.; Bouwer, S.

    2006-12-01

    Space environment research and space weather operations require solar irradiances in a variety of time scales and spectral formats. We describe the development of solar irradiance characterization using four models and systems that are also used for space weather operations. The four models/systems include SOLAR2000 (S2K), SOLARFLARE (SFLR), APEX, and IDAR, which are used by Space Environment Technologies (SET) to provide solar irradiances from the soft X-rays through the visible spectrum. SFLR uses the GOES 0.1 0.8 nm X-rays in combination with a Mewe model subroutine to provide 0.1 30.0 nm irradiances at 0.1 nm spectral resolution, at 1 minute time resolution, and in a 6-hour XUV EUV spectral solar flare evolution forecast with a 7 minute latency and a 2 minute cadence. These irradiances have been calibrated with the SORCE XPS observations and we report on the inclusion of these irradiances into the S2K model. The APEX system is a real-time data retrieval system developed in conjunction with the University of Southern California Space Sciences Center (SSC) to provide SOHO SEM data processing and distribution. SSC provides the updated SEM data to the research community and SET provides the operational data to the space operations community. We describe how the SOHO SEM data, and especially the new S10.7 index, is being integrated directly into the S2K model for space weather operations. The IDAR system has been developed by SET to extract coronal hole boundaries, streamers, coronal loops, active regions, plage, network, and background (internetwork) features from solar images for comparison with solar magnetic features. S2K, SFLR, APEX, and IDAR outputs are integrated through the S2K solar irradiance platform that has become a hybrid system, i.e., a system that is able to produce irradiances using different processes, including empirical and physics-based models combined with real-time data integration.

  16. The formation and disintegration of magnetic bright points observed by sunrise/IMaX

    Energy Technology Data Exchange (ETDEWEB)

    Utz, D.; Del Toro Iniesta, J. C.; Bellot Rubio, L. R. [Instituto de Astrofísica de Andalucía (CSIC), Apdo. de Correos 3004, E-18080 Granada (Spain); Jurčák, J. [Astronomical Institute, Academy of Sciences of the Czech Republic, 251 65 Ondřejov (Czech Republic); Martínez Pillet, V. [Instituto de Astrofísica de Canarias, Vía Láctea, s/n, E-38200 La Laguna (Spain); Solanki, S. K. [Max-Planck Institut für Sonnensystemforschung, Max-Planck-Strasse, 2, D-37191 (Germany); Schmidt, W., E-mail: utz@iaa.es, E-mail: dominik.utz@uni-graz.at [Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, D-79104 Freiburg (Germany)

    2014-12-01

    related spatially and temporally to these downflows. The paper is complemented by a detailed discussion of aspects regarding the applied methods, the complementary literature, and in depth analysis of parameters like magnetic field strength and velocity distributions. An important difference to magnetic elements and associated bright structures in active region plage is that most of the quiet Sun bright points display significant downflows over a large fraction of their lifetime (i.e., in more than 46% of time instances/measurements they show downflows exceeding 1 km s{sup –1}).

  17. Le carcinome parathyroïdien: à propos d’un cas et revue de la literature

    Science.gov (United States)

    kolsi, Naourez; Jellali, Sondos; Koubaa, Jamel

    2017-01-01

    Le carcinome parathyroïdien est une tumeur maligne, très rare, de la glande parathyroïde. Cliniquement, ce cancer se présente souvent par un tableau d'hyperparathyroïdie primaire sévère. Le diagnostic est histologique mais n'est pas toujours aisé. Le traitement est basé sur la chirurgie. Femme âgée de 59 ans, aux antécédents d'hypertension artérielle, et de lithiases rénales récidivantes, consultait pour des douleurs osseuses diffuses avec asthénie. L'examen du cou a trouvé une tuméfaction basi-cervicale dure et à bord inférieur non palpable. A la biologie: hypercalcémie à 4,1 mmol/l, une hyperparathyroïdie avec valeur de parathormone (PTH) très élevée à 1088 pg/ml soit 13 fois la normale. La scintigraphie au Technétium-99m-sestamibi a montré une plage de fixation anormale de MIBI en projection de la parathyroïde inférieure gauche. Une parathyroïdectomie inférieure gauche, avec évidement médiastino-récurrentiel homolatéral ont été réalisés. Les suites opératoires étaient marquées par la normalisation de la calcémie et de la PTH. L'anatomopathologie était en faveur d'un carcinome parathyroïdien. Le diagnostic de carcinome parathyroïdien est généralement établi sur la conjonction de signes radiologiques biologiques et histologiques. La gravité de cette pathologie est due à l'hypercalcémie sévère et au risque de récidive et de métastases à distance justifiant la surveillance prolongée. PMID:28819506

  18. Low-energy electron observation of graphite and molybdenite crystals. Application to the study of graphite oxidation; Observation au moyen d'electrons de faible energie de cristaux de graphite et de molybdenite. Application a l'etude de l'oxydation du graphite

    Energy Technology Data Exchange (ETDEWEB)

    David, G [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1969-07-01

    The LEED study of cleaved (0001) faces of crystals having a layered structure allowed to investigate flakes free of steps on graphite and molybdenite, to show twinning on natural graphite. By intensity measurements and computation in the case of a kinematical approximation it has been possible to determine an inner potential of 19 eV for graphite and to identify the direction of the Mo-S bond of the surface layer of molybdenite. The oxidation of graphite has been studied by observing changes, in symmetry of the diffraction patterns and by mass spectrometry of the gases evolved during the oxidation. No surface compounds have been detected and the carbon layers appeared to be peeled off one after the other. The oxidation took place at temperatures higher than 520 C under an oxygen pressure of 10{sup -5} torr. (author) [French] L'etude par diffraction des electrons lents des faces (0001) de cristaux ayant une structure en feuillet a permis de mettre en evidence des plages sans gradins sur des clivages de graphite et de molybdenite caracterisees par la symetrie ternaire des diagrammes, de montrer l'existence de macles sur des cristaux de graphite naturel. Un calcul utilisant une approximation cinematique a ete applique aux intensites mesurees des taches de diffraction; il a ete ainsi possible de determiner un potentiel interne de 19 eV pour le graphite et de preciser la direction de la liaison Mo-S du feuillet superficiel de la molybdenite. L'oxydation du graphite a ete etudiee en mettant en relation des changements de symetrie des diagrammes de diffraction avec l'analyse des gaz provenant de la reaction carbone-oxygene. Il a ete montre qu'il n'y avait pas formation de composes de surface et que les couches de carbone etaient enlevees les unes apres les autres. L'oxydation a ete observee sous une pression d'oxygene de 10{sup -5} torr au-dessus de 520 C. (auteur)

  19. Theoretical study of properties due to the curvature in the toroid shape in magnetohydrodynamics; Etude theorique des proprietes dues a la courbure dans les configurations toriques en magnetohydrodynamique

    Energy Technology Data Exchange (ETDEWEB)

    Adam, J C [Commissariat a l' Energie Atomique, Fontenay-aux-Roses (France). Centre d' Etudes Nucleaires

    1968-03-01

    'equilibre {nu}{<=}1 caracterisant les effets de courbure. On montre que plus {nu} est voisin de 1 plus les quantites de shear et de V{sup {phi}} qui interviennent dans le critere de stabilite seront importants. Enfin, l'etude de la stabilite met en evidence le fait que la plage de stabilite due aux effets de courbure est d'autant plus reduite que l'on se place au voisinage de L/2{pi} entier grand. (auteur)

  20. Feasibility study for the installation of a small hydro electric power plant; Etude de faisabilite. Petite centrale hydro-electrique au lieu dit 'Sous les Roches' a Sonceboz

    Energy Technology Data Exchange (ETDEWEB)

    Tissot, N. [MHyLab, Mini-Hydraulics Laboratory, Montcherand (Switzerland); Hausmann, H. [Hans Hausmann, Bevilard (Switzerland)

    2003-07-01

    This report for the Swiss Federal Office of Energy presents a technical, economical and ecological analysis of the feasibility of a small hydroelectric power plant at Sonceboz, in the Swiss Jura mountains. The power of the planed plant would typically be 500 kW for a water head of about 10 m. The study shows that, compared to one single turbine, a pair of Kaplan type turbines would be operational over a larger range of the river's water flow rate. This solution would be a little bit more costly but offer more flexibility for maintenance. Two maximum water flow rates are considered, 4.5 and 6 m{sup 3}/s respectively. According to the economical study, done with current electric kWh prices, both configurations are viable while the largest flow rate leads to a larger profit. The report is rounded up by a sensitivity analysis considering variations in annual power generation, electro-mechanical and construction cost as well as turbine efficiency. It indicates that this last factor could be crucial for the overall profitability. [French] Ce rapport est le resultat detaille de l'analyse technico-economique et ecologique de faisabilite de la realisation d'une petite centrale hydroelectrique basse chute qui pourrait exploiter une denivellation d'environ 10 m pour une puissance de l'ordre de 500 kW pres de Sonceboz dans le Jura suisse. L'etude montre que le couplage de deux turbines Kaplan offrirait une possibilite de fonctionnement sur une plus grande plage de flux ainsi qu'une plus grande flexibilite de maintenance, ceci pour un cout legerement superieur a l'option a une seule turbine. Les debits de 4.5 et 6 m{sup 3}/s sont consideres. L'etude economique montre que le debit de 6 m{sup 3}/s est plus rentable au prix de vente actuel du kWh. L'article se termine par une analyse de sensibilite sur les incertitudes concernant la production annuelle, les prix de l'electromecanique et du genie civil et le rendement des

  1. Adaptation of bacteriophages to new hosts through overcoming the interspecific barrier

    Directory of Open Access Journals (Sweden)

    Е. N. Andriychuk

    2016-10-01

    Full Text Available Four wild type phage isolates were tested on P. syringae isolated from potato tuber samples collected in the Kiev and Cherkasy regions of Ukraine. The isolated phages formed clear plaques and had a virion size of 2 to 12 nm. Electron microscopy showed that the phages were of similar size and structure and consisted of isometric particles with long tails characteristic of the Podoviridae family. The effectiveness of phage culturing on bacteria different from the original host was also studied on two phytopathogenic strains of Pseudomonas savastanoi pv. рhaseolicola 4013 and P. syringae pv. tabaci 223. However, no stable isolates could be extracted from P. savastanoi pv. phaseolicola as the plages became inactive after a few passages on the bacterial culture. In order to overcome this, the phages were first cultured on P. syringae pv. tabaci before being transferred to P. savastanoi pv. рhaseolicola. The titers obtained were compared with phage titers from the original host bacteria. Thus, it was determined that the changes occuring in phages after their transfer to the Pseudomonas strain 4013 were irreversible. The changes were evaluated by comparing the effectiveness of phage culturing after a cycle of passages on strains 4013 and 223 where the phages were adapted to strain 4013 after being cultured on strain 223. Additionally, the effectiveness of phage culturing on strain 223 was also determined. The change in the effectiveness of phage culturing for the entire phage range suggests the presence of a defensive system in bacteria when the phages were transferred from strain 223 to strain 4013. The irreversibility of the changes occuring in phages was also tested and it was determined that phages 223/4 and 7591/2 adapt to original hosts and swiftly restore their original titers. Phage 7591/1, however, showed titers that were lower than the ones obtained from the original host culture. The testing of the irreversibility of changes in phages

  2. Los vertebrados del Neogeno de la Costa Sur del Perú: ambiente sedimentario y condiciones de fosilización

    Directory of Open Access Journals (Sweden)

    1988-01-01

    Full Text Available Les fossiles de vertébrés marins sont très abondants dans les Formations Pisco et Caballas de la côte sud du Pérou [sélaciens, téléostéens, reptiles, oiseaux, mammifères (cétacés, carnivores, édentés]. Ces fossiles ont contribué à l'établissement d'une stratigraphie car ils se répartissent en sept niveaux (six dans la Formation Pisco, un dans la Formation Caballas dont l'âge va du Miocène inférieur jusqu'au sommet du Pliocène inférieur. Les vertébrés, en général, montrent un état de conservation exceptionnel les squelettes complets ou subcomplets sont très courants. L'étude sédimentologique et paléontologique (taphonomie, biologie montre que les vertébrés se sont déposés en milieu de plage. Trois types de condition de bord de mer ont été définis: • plages abritées, où se forment des lumachelles à coquilles peu brisées, parfois en position de vie. Les squelettes sont généralement complets et en connexion ou bien légèrement dissociés • plages agitées à lumachelle de coquilles brisées et os isolés • récifs où les coquilles et les os sont toujours brisés. Les niveaux à vertébrés ne montrent pas de structures tidales de flux et de reflux, ce qui semble indiquer que les marées étaient de faible amplitude. Le milieu de dépôt, peu profond (de 0 à 5 m, correspond aux zones supra et intertidales. L'existence de nombreux squelettes en connexion est la preuve d'un ensablement très rapide des cadavres (quelques jours qui semble être dû plus à l'action des vagues qu'au taux de sédimentation. Dans le second cas, les squelettes auraient été dissociés par les prédateurs. La biologie des baleines (qui se reproduisent, en général, près de la côte, celle des abondants carnivores et des oiseaux (qui sont strictement dépendants de la côte pour leur reproduction confirment le milieu de bord de mer. Par ailleurs, l'édenté de la Formation Pisco est un animal qui ne pouvait pas nager (ou

  3. Footpoint detection and mass-motion in chromospheric filaments

    Science.gov (United States)

    V, Aparna; Hardersen, P. S.; Martin, S. F.

    2013-07-01

    A quiescent region on the Sun containing three filaments is used to study the properties of mass motion. This study determines if the footpoints or end-points of the filaments are the locations from where mass gets injected into the filaments. Several hypotheses have been put forth in the past to determine how a filament acquires mass. Trapping of coronal mass in the filament channel due to condensation (Martin, 1996) and injection of mass into the filaments during magnetic reconnection (Priest, et al., 1995) are some of the speculations. This study looks for indications for injection of mass via chromospheric footpoints. The data consists of blue (Hα-0.5 Å) and red (Hα+0.5 Å) wing high resolution Hα images of the W29N37 region of the Sun taken on Oct 30, 2010, from 1200 - 1600 UT. The Dutch Open Telescope was used to obtain the data. The images are aligned and animated to see Doppler motion in the fibrils. Smaller fibrils merge to form longer ones; barbs appear and disappear in one of the long filaments and is seen moving along the length of the filament. A region with no typical filament-like absorption feature is observed to be continuously receiving mass. Fibrils appear to be converging from opposite sides along what appears to be a neutral line; mass motion is seen in these fibrils as well. An eruption occurs in a region of fibrils lumped together at the end of the first hour (1300 UT) followed by plage brightening at 1430 UT near one of the filament regions. Helioviewer (Panasenco, et al., 2011) is used for aligning the images; GIMP is used for precision alignment and animation. Each frame in the sequence is studied carefully to note changes in the filament regions. The footpoints of the filaments are determined by the changes observed in the position of the filament ‘legs’ in each frame. Variations in the magnetic polarity corresponding to changes observed in the chromosphere are analyzed using HMI magnetograms. Bright and dark points on the

  4. The Costa Maya:  Evolution of a Touristic Landscape La Costa Maya : évolution d'un paysage touristique La Costa Maya : evolución de un paisaje turístico

    Directory of Open Access Journals (Sweden)

    Klaus J. Meyer-Arendt

    2010-06-01

    Full Text Available La Costa Maya est une région côtière du sud du Quintana Roo (Mexique, proche de l'îlet Ambergris au Bélize. Contrairement à la côte caribéenne du Mexique qui a souffert du développement du tourisme de masse à Cancun et le long de la Riviera Maya, la Costa Maya s'est orientée vers un développement durable avec notamment une faible densité de construction et le développement de l'écotourisme.Le développement s'est concentré autour de Puerto Costa Maya où un terminal de croisière a été construit en 2001. La station balnéaire (balneario de Majahual est devenue dépendante des 10-12 bateaux de touristes qui débarquaient chaque semaine. En dépit d'importants plans de développement, les plages reculées de la Costa Maya accueillaient tout au plus des écotouristes aisés et du tourisme lié à la plongée sous-marine.Le cyclone Dean, de catégorie 5, a dévasté le paysage en août 2007 et le rétablissement économique n'a pu être entamé que fin 2008, après la réouverture du terminal de croisière et la reconstruction de Majahual. Fin 2009, le trafic de croisière n'a pas retrouvé son niveau d'avant Dean et la récession mondiale couplée avec la grippe porcine et les violences liées à la drogue ont fait diminuer le tourisme en provenance des Etats-Unis. On ignore à quel niveau les nouvelles infrastructures tels l'aéroport international de Tulum qui propose un itinéraire de Chetumal à la plage et le nouveau complexe hôtelier à Xahuayxel, stimuleront la Costa Maya mexicaine créant peut-être une autoroute côtière reliée à San Pedro au Bélize.The Costa Maya is a vernacular coastal region of southeastern Quintana Roo (Mexico and adjacent Ambergris Cay, Belize.  As Mexico’s Caribbean coast suffered many growth pains associated with mass tourism development in Cancun and along the Riviera Maya, the Costa Maya by contrast was projected for more sustainable development including low-density housing and

  5. Systèmes de surveillance et de contrôle des rejets d'hydrocarbures. Oléomètres Systems of Monitoring and Controlling Hydrocarbon Spills. Oleometers

    Directory of Open Access Journals (Sweden)

    Guigues F.

    2006-11-01

    Full Text Available Le choix de l'appareil à mettre en ceuvre pour doser la teneur en hydrocarbures des eaux de rejet en mer doit obligatoirement être adapté au but poursuivi. Le cahier de charges d'un tel équipement comprend dix caractéristiques : I Plage de mesure : 0 à 100 ppm d'hydrocarbures (possibilité de passer à 000 pp ; 2 Fréquence des mesures : appareil à prélèvement et analyse continus; 3 Qualité des hydrocarbures: actuellement hydrocarbures lourds et adaptabilité future aux produits raffinés; 4 Respect des normes d'analyses : mesure physique échappant aux normes du fait de l'impératif que constitue la rapidité de mesure; 5 Appareil automatique à prélèvement continu : temps de réponse inférieur à 40 s ; 6 Respect de la condition « sécurité intrinsèque »; 7 Appareil n'utilisant pas de solvant auxiliaire (pour respecter le temps de réponse; 8 Précision de la mesure : 10 % de la totalité de la plage de mesure; 9 Maintenance : réduite à sa plus simple expression; 10 Possibilité de branchement d'une « boîte noire » permettant d'effectuer les contrôles à posteriori. L'exposé brosse un tableau de certains appareils, qui ont une certaine vogue ou qui ont permis de progresser dans l'étude de la détection dés hydrocarbures contenus dans les eaux de déballastage des navires pétroliers. Le détecteur à réponse ultra-rapide (DRUR a fait l'objet d'une attention toute particulière car il satisfait aux dix conditions énoncées ci-dessus. Les résultats obtenus en Laboratoire sur des boucles de contrôle sont actuellement confirmés par ceux obtenus sur des pétroliers en service. La disponibilité d'un tel équipement paraît devoir créer les conditions nécessaires pour la mise en vigueur de la Convention de Londres 1973 et contribuera d'une manière significative à la préservation du milieu marin, tout en permettant l'expansion croissante du commerce maritime. The choice of equipment for titrating the amount of

  6. Spectral bodies, temporalised spaces: Agnès Varda's motile gestures of mourning and memorial.

    Directory of Open Access Journals (Sweden)

    Jenny Chamarette

    2011-05-01

    Full Text Available

    Abstract: This article explores the dynamics of the ‘spectre’ or ‘spectral body’ of the auteurist figure of Agnès Varda, as a means of discussing the ethical practices of mourning and memorial in two of Varda’s recent moving image works. It further elaborates on the motifs of ‘spectral bodies’ and ‘temporalised spaces’ to negotiate memorial practices between and across film viewing, filmmaking and the filmmaker. It does so using two interrelated projects by Varda; one in the realm of the plastic arts (her exhibition of 2006 entitled L’Île et elle, with a particular focus on the installation Les Veuves de Noirmoutier (The Widows of Noirmoutier, 2005 and the other in film format for cinema distribution, her most recent film, Les Plages D’Agnès (The Beaches of Agnès, 2008. Drawing upon Jacques Derrida’s notion of the spectral return, or revenant, specifically in audio-visual media, I examine the processes of spectral embodiment and motile mourning at work in these autobiographical projects. The article concludes by reflecting upon the ethical possibilities of productive nostalgia and repetitive mourning, and how these gestures and sites of longing and bereavement offer an open and ludic space for shared flows and communities of affect and memory between filmmakers, artworks and audiences.

    Résumé:

  7. Cinquante années de recherches sur les débuts de l'Aurignacien en Europe occidentale

    Directory of Open Access Journals (Sweden)

    François Djindjian

    2002-01-01

    Full Text Available Une histoire des cinquante dernières années de rechercties sur les débuts de l'Aurignacien est tentée ici. Cet historique retrace brièvement les débuts entre 1860 et 1950 de la connaissance de l'Aurignacien resituant dans leur contexte les apports respectifs de Lartet, De Mortlllet, Breuil et Peyrony. Puis, les résultats des recherches des années 1950 à 1990 des différents acteurs (D. de Sonnevllle-Bordes, F. Bordes, H. M. Movius, H. Delporte, G. Laplace, J. Hahn, N. Soler, F. Bazile, F. Champagne, etc. concernant les débuts de l'Aurignacien sont analysés à la lueur des nouvelles données de fouilles en Aquitaine (Roc de Combe, La Ferrassie, Le Facteur, Caminade, Le Flageolet I, Le Plage, en Pyrénées (Gatzarria, Cueva h/iorin, en Jura-Souabe (Geissenklosterle et sur la côte méditerranéenne (abri l\\Aochi, La Laouza, l'Arbreda, L'Esquicho-Grapaou. Les apports des recherches sur le paléoenvironnement pour la reconstitution du climat et des méthodes mathématiques et informatiques dans les années 70 à la structuration chronologique de l'Aurignacien sont développés. Les différentes données à l'origine de l'existence d'un Protoaurignacien, d'un Aurignacien 0 en Périgord, d'un Aurignacien initial et la question de l'interstratification entre Castelperronien et Aurignacien sont discutées. Les récentes critiques depuis le début des années 90 concernant la fiabilité du cadre paléoclimatique des remplissages d'abrissous- roctie et la pertinence des approches typologiques sont examinées. Les conclusions amènent l'auteur à proposer suggérer que les débuts de I'Aurignacien, encore mal connus, ne sont pas uniformes suivant les régions et dans le temps. En Europe occidentale, l'existence d'un Aurignacien initial semble prouvé sur la côte méditerranéenne de la Ligurie jusqu'en Catalogne. L'expansion aurignacienne suit alors la bordure septentrionale pyrénéenne de l'Aude jusqu'en Cantabres et en Asturies. Puis, sous

  8. Instrument for continuous supervision of the radioactivity of CO{sub 2} coolant in piles - DCCA -CO{sub 2} (1960); Dispositif de controle continu de la radioactivite du CO{sub 2} de refroidissement des piles - DCCA - CO{sub 2} (1960)

    Energy Technology Data Exchange (ETDEWEB)

    Fitoussi, L [Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    partie sont presentes des calculs theoriques en particulier sur la determination du courant d'ionisation dans une chambre d'ionisation a circulation. Cette determination tient compte de plusieurs parametres tels que la moyenne des parcours des particules {beta} dans la chambre d'ionisation, le nombre lineique de paires d'ions formees dans le gaz par ces particules {beta} en fonction de leur energie, la temperature et la pression du gaz dans la chambre d'ionisation. Dans cette meme partie sont evaluees les plages de sensibilite de l'appareillage pour les mesures dans le CO{sub 2} de refroidissement des concentrations de gaz radioactifs tels que l'argon-41 et les gaz de fission de I'uranium-235. Dans la derniere partie, sont presentes les resultats des mesures effectuees avec un tel dispositif aupres de la pile EL2, les etudes particulieres effectuees sur le CO{sub 2} de refroidissement de cette pile, les enseignements tires pendant les fonctionnement normaux et les accidents ainsi qu'une breve presentation du DCCA-CO{sub 2} qui vient d'etre mis en service a G2. La conclusion souligne les possibilites d'utilisation offertes par cet appareil. (auteur)

  9. Improvements to the properties of uranium by addition of small quantities of other metals; Ameliorations apportees a l'uranium par de faibles additions metalliques

    Energy Technology Data Exchange (ETDEWEB)

    Englander, M [Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    {sup 235}. Dans les conditions optimales de fonctionnement, un meme materiau combustible doit alors fournir un minimum de 3000 MWj/t, soit 72.10{sup 6} kWh par tonne d'uranium naturel, tout en etant porte a une temperature suffisante pour jouer efficacement son role de source de chaleur (entre 350 et 550 deg. C minimum). Or d'une facon assez surprenante, les agregats polycristallins des billettes d'uranium obtenues par coulee sous vide, ou apres filage a haute temperature, se presentent comme un ensemble de grains tres grossiers, a contours dechiquetes et irreguliers, et comportent de nombreuses marques de deformation intragranulaire (macles, lignes de glissement), accompagnees de fortes sous-structures. En plus, le spectre de la dimension des grains s'etend de quelques microns a quelques millimetres, selon les plages micrographiques examinees. Sous irradiation a ces temperatures, l'uranium metallique pur en barreaux cylindriques de diametre de l'ordre du pouce, se deforme: il se produit des fissures dans la masse, des variations de dimensions longitudinales et transversales (qui se traduisent par des peaux d'orange), soit par croissances plus ou moins directionnelles, soit par deformations superficielles qui peuvent provoquer des ruptures du materiau, de sa gaine ou des fleches suffisamment importantes pour obstruer les canaux de refroidissement. Il a ete reconnu par la suite que cette instabilite, sous l'effet des contraintes thermiques d'origine nucleaire, est due a la morphologie heterogene de l'uranium et a sa structure cristalline anisotrope (U{sub {alpha}} ou U{sub {beta}}). (auteur)

  10. State Constrained Optimal Control Applied to Supervisory Control in HEVs Commande optimale avec restrictions d’états appliquée à la supervision de l’énergie de véhicules hybrides

    Directory of Open Access Journals (Sweden)

    Pérez L.V.

    2010-02-01

    charge batterie constante est assuré juste en imposant une condition d’énergie finale fixée ou par l’introduction d’un terme additionnel dans la fonction coût qui pénalise les déviations de la variable d’état par rapport à sa valeur nominale. Par contre, nous avons considéré le cas où on permet que l’état varie librement à l’intérieur d’une plage. Ce cas conduit à un problème de commande optimale avec restrictions sur la fonction de commande et sur la variable d’état. Dans ce travail, nous décrivons les difficultés qui apparaissent quand on veut rechercher la solution des conditions d’optimalité données par le Principe du Maximum de Pontryagin et comment elles peuvent être résolues par l’utilisation de la technique appelée de Transcription Directe. Celle-ci consiste en la discrétisation dans le temps de toute la formulation du problème et en l’utilisation postérieure d’un outil de programmation non linéaire pour résoudre le problème d’optimisation à dimension finie et à grande échelle qui en résulte.

  11. El impacto de la actividad turística sobre el paisaje de La Manga del Mar Menor (Murcia

    Directory of Open Access Journals (Sweden)

    Morales Yago, Francisco José

    2013-12-01

    surgie naturellement de presque vingt kilomètres de long et moins d’un kilomètre de large, ce qui donne lieu à une confluence unique entre une mer ouverte comme la Méditerranée et une autre en forme lacunaire comme le Mar Menor. Au long de quatre décennies, cet espace singulier a été soumis à un développement urbanistique intensif lié à l’activité touristique, ce qui a provoqué de graves problèmes d’organisation du territoire, comme la mobilité ou la densification résidentielle, ainsi qu’une détérioration environnementale visible qui se traduit par la perte de zones lacustres, dunes et l’amplitude des plages. Pour toutes ces raisons, il est important d’appliquer la normative en vigueur et de planifier le futur de manière adéquate afin de permettre la récupération de cet espace et d’arrêter une détérioration progressive qui pourrait compromettre son avenir comme espace naturel et touristique de premier rang.

  12. Fabrication de transistors mono-electroniques en silicium pour le traitement classique et quantique de l'information: une approche nanodamascene

    Science.gov (United States)

    Harvey-Collard, Patrick

    Les transistors mono-electroniques (SETs) sont des dispositifs ayant un grand potentiel d'applications, comme la detection de charge ultra-sensible, la logique a basse consommation de puissance, la memoire ou la metrologie. De plus, la possibilite de pieger un seul electron et de manipuler son etat de spin pourrait permettre des applications en informatique quantique. Le silicium est un materiau interessant pour fabriquer l'ilot d'un SET. Son gap semi-conducteur permet le fonctionnement du dispositif dans le regime a un seul electron ou trou et pourrait permettre d'etendre la plage d'operation du SET en temperature en augmentant l'energie d'addition du diamant central de la valeur du gap. En outre, le silicium beneficie de plus de quarante annees d'expertise en microfabrication et d'une compatibilite avec la technologie metal--oxyde--semi-conducteur complementaire (CMOS). Cependant, la fabrication de ces dispositifs fait face a de serieuses limitations a cause de la taille nanometrique requise pour l'ilot. A ce jour, les procedes de fabrication proposes permettant l'operation a la temperature ambiante sont trop peu reproductibles pour permettre des applications a grande echelle. Dans ce memoire de maitrise, la fabrication de transistors mono-electroniques en silicium (Si-SETs) pour le traitement classique et quantique de l'information est realisee avec un procede nanodamascene. Le polissage chimico-mecanique (CMP) est introduit comme etape clef de la fabrication du transistor, permettant le controle au nanometre pres (nanodamascene) de l'epaisseur du transistor. Cet outil permet la fabrication de dispositifs ayant une geometrie auparavant impossible a realiser et ouvre la porte a l'innovation technologique. De plus, un procede de gravure du silicium par plasma a couplage inductif (ICP) est developpe pour permettre la fabrication de nanostructures de silicium sur une nanotopographie alliant le nano et le 3D. Les Si-SETs fabriques sont caracterises a basse

  13. Instrument for continuous supervision of the radioactivity of CO{sub 2} coolant in piles - DCCA -CO{sub 2} (1960); Dispositif de controle continu de la radioactivite du CO{sub 2} de refroidissement des piles - DCCA - CO{sub 2} (1960)

    Energy Technology Data Exchange (ETDEWEB)

    Fitoussi, L. [Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    . Dans la seconde partie sont presentes des calculs theoriques en particulier sur la determination du courant d'ionisation dans une chambre d'ionisation a circulation. Cette determination tient compte de plusieurs parametres tels que la moyenne des parcours des particules {beta} dans la chambre d'ionisation, le nombre lineique de paires d'ions formees dans le gaz par ces particules {beta} en fonction de leur energie, la temperature et la pression du gaz dans la chambre d'ionisation. Dans cette meme partie sont evaluees les plages de sensibilite de l'appareillage pour les mesures dans le CO{sub 2} de refroidissement des concentrations de gaz radioactifs tels que l'argon-41 et les gaz de fission de I'uranium-235. Dans la derniere partie, sont presentes les resultats des mesures effectuees avec un tel dispositif aupres de la pile EL2, les etudes particulieres effectuees sur le CO{sub 2} de refroidissement de cette pile, les enseignements tires pendant les fonctionnement normaux et les accidents ainsi qu'une breve presentation du DCCA-CO{sub 2} qui vient d'etre mis en service a G2. La conclusion souligne les possibilites d'utilisation offertes par cet appareil. (auteur)

  14. La visita de empresa, otra forma de hacer turismo

    Directory of Open Access Journals (Sweden)

    Zárate Martín, M. Antonio

    2011-06-01

    loisir et inactivité ou «tourisme de soleil et de plage». Tout à la fois, les activités culturelles sont en train de devenir en tête dans les motivations des touristes et l’emploi de leur temps libre. C’est dans ce contexte que la «visite d’entreprise» mérite d’être associée au tourisme culturel et au «tourisme de style de vie». Plus encore, la «visite d’entreprise» rejoigne le «tourisme actif» du moment où on y meut en jeu la communication, les expériences, l’échange d’idées, la découverte des «savoir-faire» et l’introduction de nouveaux services. Par ailleurs, la «visite d’entreprise» contribue à l’embauche de salariés et au développement local. Les entrepreneurs concernés y trouvent toujours un moyen de vanter leurs produits et de grandir leurs chiffres d’affaires.

  15. Aerodynamic and thermal studies of cans of gas cooled fuel elements; Etudes aerodynamiques et thermiques de gaines d'elements combustibles refroidis par gaz

    Energy Technology Data Exchange (ETDEWEB)

    Gelin, P [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires; Milliat, J P [Electricite de France (EDF), 75 - Paris (France)

    1964-07-01

    l'amelioration des grappes et s'est ensuite poursuivie dans les deux Laboratoires pour le refroidissement interne des elements combustibles annulaires. Au fur et a mesure de l'avancement de ces etudes, les moyens d'essais se sont amplifies tandis que les methodes experimentales n'ont cesse de s'ameliorer. Actuellement, les deux Laboratoires, qui travaillent en pleine collaboration, disposent de moyens puissants. Pour les grappes, l'effort a surtout porte sur les pertes de charge dues aux pieces d'assemblage et sur les variations de temperature autour des elements de la grappe. On est arrive ainsi a determiner d'une facon satisfaisante les points chauds de gaine, les deformations des crayons et les conditions de stabilite de ces deformations. Pour les gaines a chevrons, les etudes ont porte, d'une part sur l'evolution des performances en fonction des parametres geometriques, et, d'autre part sur les singularites aerodynamiques et thermiques creees tant par les ailettes que par les interruptions de cartouche. Ces etudes ont abouti a une connaissance tres complete des cartouches choisies pour les reacteurs EDF2 et EDF3, et ouvrent maintenant des perspectives tres encourageantes pour les reacteurs a venir, en particulier les reacteurs equipes d'elements annulaires; parmi les solutions convenant a la gaine interne de l'element annulaire, les corrugations et les ailettes longitudinales ont fait l'objet d'essais assez etendus dans une large plage de nombre de Reynolds. (auteurs)

  16. Solar Tutorial and Annotation Resource (STAR)

    Science.gov (United States)

    Showalter, C.; Rex, R.; Hurlburt, N. E.; Zita, E. J.

    2009-12-01

    efficient in similar astrophysical projects (e.g. the “Galaxy Zoo.”) For “crowdsourcing” to be effective for solar research, the public needs knowledge and skills to recognize and annotate key events on the Sun. Our tutorial can provide this training, with over 200 images and 18 movies showing examples of active regions, coronal dimmings, coronal holes, coronal jets, coronal waves, emerging flux, sigmoids, coronal magnetic loops, filaments, filament eruption, flares, loop oscillation, plage, surges, and sunspots. Annotation tools are provided for many of these events. Many features of the tutorial, such as mouse-over definitions and interactive annotation examples, are designed to assist people without previous experience in solar physics. After completing the tutorial, the user is presented with an interactive quiz: a series of movies and images to identify and annotate. The tutorial teaches the user, with feedback on correct and incorrect answers, until the user develops appropriate confidence and skill. This prepares users to annotate new data, based on their experience with event recognition and annotation tools. Trained users can contribute significantly to our data analysis tasks, even as our training tool contributes to public science literacy and interest in solar physics.

  17. Comportement des métaux et fonctionnement d’un estuaire en zone sub aride : cas de l’estuaire du Souss (côte atlantique Marocaine

    Directory of Open Access Journals (Sweden)

    Elmouden, A.

    2005-04-01

    des teneurs en métaux dans les carottes montre un enrichissement dans les horizons à granulométrie fine attribué une migration des métaux par diagenèse précoce et leurs rétention dans les couches argileuses, et aussi probablement au contrôle par les conditions oxydo-réductrices du milieu. L’estuaire du Souss ne joue pas donc un rôle de piége vis-à-vis des métaux polluants comme c’est le cas de nombreux estuaires des zones tempérées. Par contre, la colonne sédimentaire de la slikke enregistre une légère augmentation des teneurs en éléments métalliques qui pourraient constituer un risque pour la vie aquatique et pour la salubrité des plages environnantes, en cas de changement des conditions physico-chimiques du milieu

  18. Extension of the Single-Event Methodology to Metal Catalysis: Application to Fischer-Tropsch Synthesis Extension de la méthodologie des événements constitutifs à la catalyse métallique : Application à la synthèse Fischer-Tropsch

    Directory of Open Access Journals (Sweden)

    Lozano-Blanco G.

    2010-10-01

    Full Text Available The single-event methodology has been extended to metal catalysis using Fischer-Tropsch synthesis on an iron-based catalyst as case study. The reaction mechanism has been assessed in terms of elementary steps that could be categorized in reaction families such as reductive elimination, β-hydride elimination and methylene insertion. A computer code has been developed for the generation of the reaction network containing these elementary steps. The representation of reacting and intermediate species explicitly takes into account metal-carbon bonds as well as the presence of oxygen. The model has been validated using iron-based catalytic data at 623 K, 0.6 to 2.1 MPa, inlet molar H2/CO ratio between 2 and 6. 14 parameters, among which 10 activation energies and 4 atomic chemisorption enthalpies have been adjusted to the experimental data. Experimentally observed trends in alkane and 1-alkene product yields with the carbon number were adequately reproduced as well as the individual molar yields of the non-hydrocarbon products. La méthodologie par événements constitutifs a été étendue à la catalyse métallique en utilisant la synthèse Fischer-Tropsch sur un catalyseur au fer comme cas d'étude. Le mécanisme réactionnel a été décomposé en étapes élémentaires qui peuvent être classées par type de réactions, telles que l'élimination réductrice, l'élimination d'hydrure en β, et l'insertion de groupe méthylène. Un code de calcul a été développé pour générer le réseau réactionnel impliquant ces étapes élémentaires. La représentation des réactifs et des espèces intermédiaires prend en compte explicitement les liaisons carbone-métal et inclut la présence d'atomes d'oxygène. Le modèle a été validé sur une base de données obtenues sur un catalyseur à base de fer à 623 K, sur une plage de 0,6 à 2,1 MPa, un ratio H2/CO en entrée variant de 2 à 6. Quatorze paramètres, dont 10 énergies d'activation et 4

  19. Sediment depositions upstream of open check dams: new elements from small scale models

    Science.gov (United States)

    Piton, Guillaume; Le Guern, Jules; Carbonari, Costanza; Recking, Alain

    2015-04-01

    numbers that the flows tend to adopt? New small scale model experiments have been undertaken focusing on depositions processes and their related hydraulics. Accurate photogrammetric measurements allowed us to better describe the deposition processes3. Large Scale Particle Image Velocimetry (LS-PIV) was performed to determine surface velocity fields in highly active channels with low grain submersion4. We will present preliminary results of our experiments showing the new elements we observed in massive deposit dynamics. REFERENCES 1.Armanini, A., Dellagiacoma, F. & Ferrari, L. From the check dam to the development of functional check dams. Fluvial Hydraulics of Mountain Regions 37, 331-344 (1991). 2.Piton, G. & Recking, A. Design of sediment traps with open check dams: a review, part I: hydraulic and deposition processes. (Accepted by the) Journal of Hydraulic Engineering 1-23 (2015). 3.Le Guern, J. Ms Thesis: Modélisation physique des plages de depot : analyse de la dynamique de remplissage.(2014) . 4.Carbonari, C. Ms Thesis: Small scale experiments of deposition processes occuring in sediment traps, LS-PIV measurments and geomorphological descriptions. (in preparation).

  20. Open-air ionisation chambers with walls of soft-tissue equivalent material for measuring photon doses; Chambres d'ionisation d'ambiance a parois en materiau equivalent aux tissus mous pour la mesure des doses absorbees dues aux photons

    Energy Technology Data Exchange (ETDEWEB)

    Vialettes, H.; Anceau, J.C.; Grand, M.; Petit, G. [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1968-07-01

    'energie comprise entre 10 keV et 10 MeV. De plus, ce materiau ne contenant pas d'hydrogene, la chambre presente une sensibilite aux neutrons nettement plus faible que les autre chambres couramment utilisees. Enfin, la forme de ces chambres a ete etudiee pour obtenir une reponse en isotropie satisfaisante; c'est ainsi que pour un rayonnement gamma de 27 keV, la chambre de volume 3 litres est isotrope a 10 pour cent pres sur 270 degres, et celle de volume 12 litres est isotrope a 10 pour cent pres sur 300 degres ; pour un rayonnement gamma de 1.25 MeV, cette plage s'etend sur 330 degres pour la chambre de 3 litres, et 360 degres pour la chambre de 12 litres. Ce rapport presente les mesures effectuees sur ces chambres ainsi que les resultats obtenus. Ces resultats sont ensuite compares a ceux obtenus avec les autres chambres utilisees couramment dans le domaine de la radioprotection. (auteurs)

  1. Testing of a reactimeter for a light water reactor in the range + 500 to - 5000 pcm; Essai d'un reactimetre pour reacteur a eau legere dans la gamme + 500, - 5000 pcm

    Energy Technology Data Exchange (ETDEWEB)

    Chauvet, G [Commissariat a l' Energie Atomique, Grenoble (France). Centre d' Etudes Nucleaires

    1964-07-01

    calcul de la reactivite ne repose pas sur un asservissement. Un de ses inconvenients est de ne pas pouvoir fonctionner en dehors d'une plage de variation de la puissance excedant 2,5 decades. Mais la mesure d'un echelon negatif de reactivite entre 0 et 3000 pcm est immediate. Il mesure la reactivite en ne la deduisant pas de la periode; il indique donc la reactivite d'une maniere precise en divergence aussi bien qu'en convergence, regime ou il n'existe pas, a proprement parler, de periode. Il permet donc un etalonnage tres rapide des barres de controle d'un reacteur (methode de rod-drop), la mesure de la reactivite d'une manipulation inseree dans le coeur, la mesure de certains effets de temperature. En inserant 'au moteur' une barre de controle dans le coeur, on peut tracer directement sa courbe d'efficacite. (auteur)

  2. Systèmes multimatériaux – Assemblage par collage Multimaterial systems – Adhesive bonding

    Directory of Open Access Journals (Sweden)

    Zuanna C. Dalla

    2013-11-01

    Full Text Available L'assemblage par collage multimatériaux (métal/composite, métal/verre, métal/plastiques, verre/plastiques… offre de nombreux avantages par rapport aux techniques d'assemblages traditionnelles (pas d'affaiblissement des matériaux par la température, tenues en fatigue et à la corrosion améliorées, esthétisme, étanchéité…. Cependant la qualité et la durabilité à long terme des assemblages collés dépendent d'une bonne conception de ces assemblages : Le choix de préparations de surfaces efficaces, robustes, facilement industrialisables et respectueuses de l'environnement, Le choix d'adhésifs aptes à répondre au cahier des charges fonctionnel de l'assemblage (performances mécaniques, thermiques, chimiques… dont la mise en œuvre est compatible avec les contraintes d'industrialisation (cadences, temps de manipulation des pièces, environnement du poste collage…, Le dessin et le dimensionnement de la liaison de façon à transmettre les efforts mécaniques spécifiés dans la plage de températures de fonctionnement des pièces collées (en tenant compte des dilatations différentielles des matériaux assemblés. Cette démarche sera développée en donnant l'état de l'art actuel et les avancées les plus récentes sur les trois thèmes cités ci-dessus. Adhesive-bonding offers many advantages over traditional joining techniques (no weakening of materials by temperature, required fatigue and improved corrosion resistance, aesthetics, sealing… for multimaterial assembly (metal/composite, metal/glass, metal/plastic, glass/plastic…. However the quality and long term durability of bonded assemblies depend on a correct design of the joint: Choice of eco-efficient surfaces preparations, robust, and easily processed, Choice of adhesive in good adequation with the functional specifications of the assembly (mechanical performance, thermal, chemical… whose implementation is compatible with industrialization constraints

  3. Fluctuations Magnetiques des Gaz D'electrons Bidimensionnels: Application AU Compose Supraconducteur LANTHANE(2-X) Strontium(x) Cuivre OXYGENE(4)

    Science.gov (United States)

    Benard, Pierre

    Nous presentons une etude des fluctuations magnetiques de la phase normale de l'oxyde de cuivre supraconducteur La_{2-x}Sr _{x}CuO_4 . Le compose est modelise par le Hamiltonien de Hubbard bidimensionnel avec un terme de saut vers les deuxiemes voisins (modele tt'U). Le modele est etudie en utilisant l'approximation de la GRPA (Generalized Random Phase Approximation) et en incluant les effets de la renormalisation de l'interaction de Hubbard par les diagrammes de Brueckner-Kanamori. Dans l'approche presentee dans ce travail, les maximums du facteur de structure magnetique observes par les experiences de diffusion de neutrons sont associes aux anomalies 2k _{F} de reseau du facteur de structure des gaz d'electrons bidimensionnels sans interaction. Ces anomalies proviennent de la diffusion entre particules situees a des points de la surface de Fermi ou les vitesses de Fermi sont tangentes, et conduisent a des divergences dont la nature depend de la geometrie de la surface de Fermi au voisinage de ces points. Ces resultats sont ensuite appliques au modele tt'U, dont le modele de Hubbard usuel tU est un cas particulier. Dans la majorite des cas, les interactions ne determinent pas la position des maximums du facteur de structure. Le role de l'interaction est d'augmenter l'intensite des structures du facteur de structure magnetique associees a l'instabilite magnetique du systeme. Ces structures sont souvent deja presentes dans la partie imaginaire de la susceptibilite sans interaction. Le rapport d'intensite entre les maximums absolus et les autres structures du facteur de structure magnetique permet de determiner le rapport U_ {rn}/U_{c} qui mesure la proximite d'une instabilite magnetique. Le diagramme de phase est ensuite etudie afin de delimiter la plage de validite de l'approximation. Apres avoir discute des modes collectifs et de l'effet d'une partie imaginaire non-nulle de la self-energie, l'origine de l'echelle d'energie des fluctuations magnetiques est examinee

  4. Description of a Reactivity Measuring Apparatus; Description d'un Type d'Appareil de Mesure de la Reactivite

    Energy Technology Data Exchange (ETDEWEB)

    Deiss, M.; Uberschlag, J. [Centre d' Etudes Nucleaires de Saclay (France)

    1966-06-15

    derniere structure realise l'inversion de l'operateur mathematique definissant la fonction du reacteur. Celle-ci a ete retenue pour la realisation des deux appareils decrits. Elle permet d'adapter a ceux-ci les qualites propres aux systemes asservis et notamment l'action de filtrage des bruits de haute frequence, L'organe de sortie de ces divers types d'appareils est constitue par un diviseur extrayant le terme Greek-Small-Letter-Delta K du produit N Greek-Small-Letter-Delta K fourni par le premier etage de l'appareil. Les deux appareils different entre eux par la nature de l'organe de sortie constitue par un diviseur, soit potentiometrique, soit electronique. Le premier de ces appareils convient en principe dans la plupart des cas habituels de mesure. Le second en raison de son temps de reponse plus reduit est adapte i la mesure en divergence de reactivites de valeurs plus elevees, ainsi qu'a des mesures en convergence, meme sur des plages de puissance limitees. (author)

  5. PREMIÈRE CARACTÉRISATION MORPHOLOGIQUE, BIOLOGIQUE ET GÉNÉTIQUE DES POPULATIONS DE GRANDE ALOSE (ALOSA ALOSA ET D’ALOSE FEINTE (ALOSA FALLAX SPP. DE LA CHARENTE (FRANCE.

    Directory of Open Access Journals (Sweden)

    VÉRON V.

    2001-07-01

    Full Text Available Les deux espèces d’aloses atlantiques (Alosa alosa et A. fallax colonisent la Charente mais leurs populations n’ont jamais été décrites à la différence de celles des grands fleuves français voisins. Les propriétés physiques du bassin sont présentées en terme de qualité de l’eau, d’habitats et d’obstacles à la migration. Les grandes aloses colonisent la Charente jusqu’en amont d’Angoulême (171 km lorsque les conditions hydrauliques des mois d’avril et mai effacent les 21 barrages situés en aval. Des frayères actives ont été localisées sur cette portion du fleuve. Les aloses feintes sont bloquées plus en aval par le barrage de Crouin (102 km, aval de Cognac et une seule frayère active a été repérée. L’abondance de ces deux stocks d’alose ne peut pas être estimée car les seules données disponibles, faute de dispositifs de contrôle des migrations, proviennent des captures faites par pêche professionnelle et à la ligne. La caractérisation morphologique et génétique des deux espèces a été faite à partir de comptages méristiques, de mesures morphométriques et de prélèvements (écaille, tissus et sang réalisés en 1997 et 1998. Le nombre total moyen de branchiospines du premier arc branchial gauche chez les grandes aloses est de 125 contre 42 chez les feintes. Quelle que soit l’espèce et à âge égal, les femelles ont une taille moyenne supérieure à celle des mâles. Les femelles de grande alose sont âgées en moyenne de 5 ans et les mâles de 4 ans, aucun des poissons échantillonnés ne présentant de marques de reproduction antérieure. Les femelles et les mâles d’alose feinte sont âgés en moyenne de 3 ans, 12,5 % des femelles se sont déjà reproduites une fois et 3,5 % deux fois. Chez les mâles, 40 % se sont déjà reproduits une fois. La plage temporelle de reproduction a été déterminée par suivi de terrain et enquête. Celle des grandes aloses se situe entre la premi

  6. Patterns in groundwater chemistry resulting from groundwater flow

    Science.gov (United States)

    Stuyfzand, Pieter J.

    qualité de l'eau vers une absence de fluctuations, de polluées vers non polluées, d'acides vers basiques, d'oxygénées vers anoxiques et méthanogènes, depuis des échanges de base inexistants vers des échanges significatifs, de l'eau douce vers l'eau saumâtre. Ceci est montré pour une nappe d'eau douce dans une dune côtière des Pays-Bas. Dans "l'hydrosome", on montre que la disparition du carbonate de calcium par lessivage à plus de 15m et celle de cations adsorbés d'origine marine (Na+, K+ et Mg2+) à plus de 2500m vers l'aval-gradient correspond à environ 5000 ans d'écoulement, depuis que la barrière de la plage avec les dunes s'est mise en place. Les zones d'alimentation ponctuelle dans les dunes sont mises en évidence par l'eau souterraine montrant une plus faible évolution prograde de sa qualité que l'eau souterraine de la dune alentour. L'eau du Rhin utilisée pour la réalimentation artificielle dans les dunes a fourni des types hydrochimiques distincts, qui marquent l'écoulement, le mélange et les âges de l'eau souterraine. Resumen El flujo subterráneo tiene una gran importancia sobre la hidroquímica de un sistema ya que reduce la mezcla por difusión, transporta las huellas químicas y biológicas de las acciones antrópicas en la zona de recarga y drena el sistema acuífero. Las tendencias globales vienen regidas por las diferencias en el flujo de agua meteórica que atraviesa el subsuelo. En un hidrosoma individual (cuerpo de agua de un origen específico), se suele desarrollar la siguiente línea de evolución (secuencia de facies) en la dirección del flujo: de gran a nula fluctuación en la calidad del agua, de agua contaminada a no contaminada, de ácida a básica, de óxica a anóxica-metanogénica, de nulo a importante cambio de base y de agua dulce a salobre. Esto puede verse, por ejemplo, en las aguas dulces presentes en las dunas costeras de Holanda. En este hidrosoma, el lixiviado de carbonato cálcico, hasta 15m, y de

  7. Fuel material neutron crystallography texture and structure determinations (1960); Etudes sur l'evolution des structures cristallines de l'uranium par neutrocristallographie (1960)

    Energy Technology Data Exchange (ETDEWEB)

    Laniesse, J; Englander, M; Meriel, P [Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    }, la transformation {beta} {yields} {alpha} peut etre suivie en fonction du temps et a des temperatures telles que les taux de comptages ainsi que leurs frequences soient suffisants. A titre d'exemple, dans la presente communication, les resultats obtenus sur des echantillons d'uranium pur file a 600 deg. C avec un rapport de plage egal a 10,4 et sur des echantillons ayant subi ensuite 4 recuits a 700 deg. C interrompus par 4 trempes a l'eau, sont exprimes, ainsi que l'equation regissant la cinetique de transformation allotropique {beta} {yields} {alpha} a la temperature de 333 deg. K d'un alliage massif d'U contenant 1000 parties par million de Cr. (auteur)

  8. Contribution to the study and use of ionisation chambers for nuclear reactor control (1965); Contribution a l'etude et a l'utilisation des chambres d'ionisation pour le controle des reacteurs nucleaires (1965)

    Energy Technology Data Exchange (ETDEWEB)

    Duchene, J [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1961-02-15

    high-power reactors. (author) [French] Les chambres d'ionisation sont actuellement les detecteurs les mieux adaptes au controle des reacteurs nucleaires par des mesures neutroniques. Nous avons cru bon de rappeler quelques generalites concernant la dynamique des reacteurs, les differents procedes de detection des neutrons, le fonctionnement des chambres d'ionisation et les methodes de mesure utilisees. Notre contribution aux techniques de controle des reacteurs consiste d'une part en une tentative de synthese des facteurs intervenant dans le fonctionnement des chambres d'ionisation, l'etude de ces facteurs, et d'autre part l'elaboration de chambres d'ionisation a fission et a bore permettant de suivre la marche d'un reacteur du demarrage jusqu'a la puissance maximale. Dans le domaine des chambres a fission, nous avons en particulier ameliore les techniques de depot d'oxyde d'uranium sur l'aluminium et realise la mise au point de depots par electrolyse sur d'autres metaux: acier inoxydable, cuivre, molybdene, nickel, tantale, titane, kovar, tungstene et beryllium. Nous avons elabore plusieurs types de chambres a fission servant au demarrage des reacteurs: un type de performances moyennes actuellement utilise dans les piles francaises un type a haute sensibilite un type a haute temperature qui a fonctionne jusqu'a 600 deg. C. En ce qui concerne les chambres a bore, nous avons etudie les perturbations apportees dans les mesures par l'exposition des chambres a d'importants flux de neutrons et a un rayonnement {gamma} intense. Cette exposition produit une modification des proprietes des materiaux constitutifs et la production dans les chambres d'un bruit de fond qui peut gener considerablement les mesures neutroniques. Nous avons montre que la technique de compensation permettait de limiter l'importance de ce bruit de fond et d'augmenter ainsi la plage de fonctionnement des chambres d'ionisation classiques destinees aux mesures de puissance. Enfin, nous avons realise deux

  9. Hydrothermal Dolomites in the Early Albian (Cretaceous Platform Carbonates (NW Spain: Nature and Origin of Dolomites and Dolomitising Fluids Dolomies hydrothermales présentes dans les carbonates de la plate-forme albienne précoce (Crétacé; NO de l’Espagne : nature et origine des dolomies et des fluides dolomitisants

    Directory of Open Access Journals (Sweden)

    Shah M.M.

    2012-02-01

    hydrodynamic fluid flow along the faults/fractures in the Albian carbonate platform. Subsequently, a second episode of very hot and localised dolomitisation may be related to igneous activity and convective flow. La présente étude décrit les variations temporelle et spatiale des signatures pétrographiques et géochimiques des corps dolomitiques liés aux failles dans les régions de Ranero et El-Moro (vallée de Karrantza, montagnes cantabriques; NO de l’Espagne. Ces corps dolomitiques se trouvent dans les carbonates albiens, déposés dans le bassin Basque-Cantabrique suite à une subsidence intense liée au rift comportant un système de failles associé suivant des orientations diverses. Des circulations de fluides ont généré des dolomies de remplacement et de cimentation, paragénétiquement suivies de divers ciments calcitiques. Des travaux de pétrographie, minéralogie et géochimie (DRX, ICP, XRF, isotopes stables de O/C et du Sr ont aidé à distinguer les étapes hydrothermales. Deux faciès majeurs de dolomies ont été observés selon leur teneur en Fe. Les dolomies précoces sont ferrifères et remplacent le calcaire de façon plus significative que les dolomies non-ferrifères tardives. Les dolomies sont généralement stoechiométriques (de 49,76 à 51,59 % en moles de CaCO3 et présentent une large plage de valeurs de δ18O (de –18,7 à –10,5 ‰ V-PDB, ce qui pourrait indiquer une dolomitisation à phases multiples et/ou des degrés différents de recristallisation. Les valeurs de δ18O décroissantes se trouvent en corrélation avec la diminution de la teneur en Fe dans les dolomies. Dans la région de Ranero, les dolomies présentent des valeurs de δ13C légèrement moins réduites (de –0,15 à  +2,13 ‰ V-PDB que la signature de δ13C du calcaire hôte, tandis que ces valeurs sont nettement plus réduites dans la région de El-Moro (jusqu’à – 2,18 ‰ V-PDB. Les calcites hydrothermales antérieures à la dolomitisation présentent des

  10. Préface

    Science.gov (United States)

    Chardonnet, Christian; Millot, Guy

    2006-10-01

    COLOQ, réunion nationale biennale initiée en 1988 par la communauté française des lasers, de l'optique non linéaire et de l'optique quantique atteint sa neuvième édition. Depuis sa création, les objectifs poursuivis sont les suivants : - réunir la communauté française des lasers, de l'optique non linéaire et de l'optique quantique, en dépassant les clivages fondamental/appliqué, recherche publique/industrielle, - faire le point sur les avancées récentes, - permettre aux jeunes chercheurs de se rencontrer, de s'exprimer et de s'aguerrir au plan national. Le but est que tout thésard du domaine de l'optique puisse participer à COLOQ une fois durant sa thèse, présenter son travail et de se confronter à la communauté de l'optique. COLOQ9 s'est tenu, pour sa 9e édition, sur le campus universitaire de Dijon, du 7 au 9 septembre 2005. Il a été une grande réussite : nombre de participants (255) et de présentations scientifiques record (148 affiches), forte représentation des industriels (15) et participation d'environ 200 lycéens aux conférences grand public. Le nombre plus élevé que prévu d'affiches a rendu un peu serrée leur présentation : une attention particulière sera portée à cet aspect lors des prochaines éditions. Ces journées ont été consacrées à des conférences invitées données par des scientifiques de haut niveau et à des présentations sous forme d'affiches. Une plage de temps importante a été réservée pour des discussions autour des affiches. À proximité immédiate de la salle de conférence, l'exposition de matériels spécialisés pour les lasers, l'optique et l'optoélectronique a été une occasion pour les jeunes participants de découvrir et contacter les industriels et les autres grands acteurs de l'optique. L'année 2005 ayant été l'année mondiale de la physique, COLOQ9 a retenu comme thème central ”1905-2005 : à propos d'Einstein". Plusieurs grandes conférences ont été dédiées à ce th

  11. Analysis of Scan Records with a Recording Densitometer - The ''Re-Scanner''; Etude d'un Grand Collimateur a Focalisation et Fort Pouvoir de Resolution: Resultats; Analiz skenogramm s pomoshch'yu registriruyushchego densitometra - ''re-skenner''; Diseno y Funcionamiento de un Gran Colimador Enfocado de Alto Poder de Resolucion

    Energy Technology Data Exchange (ETDEWEB)

    Harris, C. C.; Bell, P. R.; Satterfield, M. M.; Ross, D. A.; Jordan, J. C. [Oak Ridge National Laboratory, TN (United States)

    1964-10-15

    assistance in the interpretation of scan records. (author) [French] U s perfectionnements des appareils de scintigraphie n'ont pas eu d'effet comparable sur le plan clinique, surtout en raison des imperfections des enregistrements scintigraphiques. En vue d'ameliorer la visualisation et le contraste des scintigrammes, on a mis au point divers appareils d'analyse. Les auteurs ont concu un densitometre enregistreur, assez simple et relativement peu couteux, qui permet de 'scintigraphier' les scintigrammes. Une cellule photoelectrique explore le scintigramme, tout comme un detecteur ascintillation explore le patient. Les impulsions a la sortie de l'appareil sont proportionnelles a la densite du scintigramme et elles peuvent etre utilisees pour etablir un nouvel enregistrement. La surface du scintigramme pour laquelle on integre les informations est determinee par l'ouverture de la c ellule . La gamme etendue des impulsions a la sortie (de zero a 15 000 impulsions/s) permet d'amplifier fortement et a volonte le contraste. Un dispositif special permet de choisir a l'avance un ' seuil de coupure' L'operation est rapide, si bien qu'un scintigramme peut etre explore en une fraction du temps qui avait ete necessaire pour l'etablir. L*etude de scintigrammes cliniques de presque tous les organes ou regions interessants a permis de constater que le densitometre enregistreur revele des informations qui n'apparaissaient pas clairement sur le scintigramme. Cet appareil a ete particulierement utile pour determiner la signification statistique de legeres variations du taux de comptage dans un scintigramme. Pour les scintigrammes representant de fortes variations de la radioactivite, ou un seul seuil de coupure du densitometre ne donne pas une image satisfaisante de toutes les zones interessantes, il fallait autrefois faire plusieurs explorations avec differents seuils de coupure. Pour surmonter cette difficulte, on a eu recours a une c ellule a deux plages qui explore le scintigramme autour

  12. Petrographical and Geochemical Study of a Kimmeridgian Organic Sequence (Yorkshire Area, Uk Étude pétrographique et géochimique d'une séquence organique du Kimmeridgien (région du Yorkshire, Angleterre

    Directory of Open Access Journals (Sweden)

    Belin S.

    2006-11-01

    les variations de nature et de teneur des divers constituants du sédiment, organiques et minéraux. Plusieurs approches analytiques ont été pratiquées à partir des mêmes échantillons : la pétrographie minérale et organique, la minéralogie, la géochimie organique. La microscopie électronique à balayage (MEB en mode électrons rétrodiffusés (ER a été privilégiée parce qu'elle constitue une méthode de choix pour l'investigation, à l'échelle du micron, de la texture organo-minérale (Krinsley et Manley, 1989; White et al. , 1984 ; Belin, 1992. Tout au long de la séquence, la composition minéralogique présente des variations limitées (fig. 1. Les constituants majeurs du sédiment sont : les argiles, la calcite, le quartz, la matière organique et la pyrite. Le cortège argileux, pratiquement invariant, se compose de kaolinite, d'illite et d'interstratifiés illite-smectite. La kaolinite est principalement détritique, alors que l'illite et les interstratifiés sont diagénétiques (Herbin et al. , 1991. La phase carbonatée est constituée essentiellement d'une population monospécifique de coccolithes (Gallois, 1976 et de débris de foraminifères. La phase siliceuse, dont la teneur est invariante dans tout le cycle, est composée de quartz détritique, dont les grains sont de petite taille (< 20 µm, et de quartz diagénétique : auréoles de néoformation autour de certains quartz détritiques, grandes plages automorphes de quartz (100 µm, épigénies de coquilles de calcite en quartz et sphérolites de calcédonite. La pyrite, diagénétique, se présente soit sous la forme de framboïdes, isolés ou en grappes, d'environ 10µm de diamètre, associés à la matière organique, soit en cristaux euhédraux. Sa quantité décroit du début à la fin du cycle considéré et elle est d'autant plus abondante qu'il y a plus de matière organique dans le sédiment. Le carbone organique total (COT mesuré par pyrolyse Rock-Eval présente des valeurs