WorldWideScience

Sample records for plages

  1. Plage

    Science.gov (United States)

    Murdin, P.

    2000-11-01

    A region of intensified emission in the solar chromosphere. Plages are revealed in monochromatic images obtained in the light of various emission lines, for example, the hydrogen-α line and the `H' and `K' lines of ionized calcium. The name derives from the French word for `beach', an allusion to the fact that these features stand out like bright sandy beaches against the fainter background of th...

  2. Spicule Dynamics over Plage Region

    CERN Document Server

    Anan, Tetsu; Kawate, Tomoko; Matsumoto, Takuma; Ichimoto, Kiyoshi; Shibata, Kazunari; Hillier, Andrew; Otsuji, Kenichi; Watanabe, Hiroko; UeNo, Satoru; Nagata, Shin'ichi; Ishii, Takako T; Komori, Hiroyuki; Nishida, Keisuke; Nakamura, Tahei; Isobe, Hiroaki; Hagino, Masaoki

    2010-01-01

    We studied spicular jets over a plage area and derived their dynamic characteristics using Hinode Solar Optical Telescope (SOT) high-resolution images. The target plage region was near the west limb of the solar disk. This location permitted us to study the dynamics of spicular jets without the overlapping effect of spicular structures along the line of sight. In this work, to increase the ease with which we can identify spicules on the disk, we applied the image processing method `MadMax' developed by Koutchmy et al. (1989). It enhances fine, slender structures (like jets), over a diffuse background. We identified 169 spicules over the target plage. This sample permits us to derive statistically reliable results regarding spicular dynamics. The properties of plage spicules can be summarized as follows: (1) In a plage area, we clearly identified spicular jet features. (2) They were shorter in length than the quiet region limb spicules, and followed ballistic motion under constant deceleration. (3) The majorit...

  3. SOUS LE PAVÉ: LA PLAGE!

    DEFF Research Database (Denmark)

    Clemmensen, Thomas Juel

    2017-01-01

    around something that could be labeled geologic resonance: The ability of a creative work or an area to bring humans on wavelengths with geology’s ‘deep time.’ When the avant-garde art movement the Situationists used the slogan ‘sous les pavés: la plage!’ the beach was associated with the free natural...... space in contrast to the paved street, which represented the suppressing power of society. But the slogan can also remind us of geology’s omnipresent character. Geology is right at our feet in and below the hard surfaces of the city, and we do not need to visit geological sights to experience geologic...

  4. Two-component model of solar plages

    Institute of Scientific and Technical Information of China (English)

    LI; Jianping(李建平); DING; Mingde(丁明德); FANG; Cheng(方成)

    2002-01-01

    By use of the 2-m Mcmath-Pierce telescope at Kitt Peak, the high-quality spectra of a plage with moderate brightness near the center of solar disk were obtained. The data include seven spectral lines, which are Hα, Hβ, CaII H and K lines and the infrared triplet. With the consideration of fine structures of solar plages, a two-component atmospheric model is constructed by keeping the cool component to be the quiet atmosphere. Three cases of the hot component are given for different filling factors where the temperature and density distribution are adjusted in order to reproduce the seven observed spectral profiles. We also briefly discuss the influence of the column density at the base of the corona, m0, and the macro-turbulent velocity on the required filling factor and computed profiles. The two-component model is compared with precious one-component semi-empirical models. The limitation of the model is pointed out and further improvement is indicated.

  5. Semi-empirical model of solar plages

    Institute of Scientific and Technical Information of China (English)

    FANG; Cheng

    2001-01-01

    [1] Zirin, H., Astrophysics of the Sun, Chapter 7, Cambridge: Cambridge University Press, 1988.[2] Shine, R. A., Linsky, J. L., Physical properties of solar chromospheric plages II. Chromospheric plage models, Solar Phys., 1974, 39: 49.[3] Kelch, W. L., Linsky, J. L., Physical properties of solar chromospheric plages III. Models based on CaII and MgII observations, Solar Phys., 1978, 58: 37.[4] Lemaire, P., Goutlebroze, J. C., Vial, J. C. et al., Physical properties of the solar chromosphere deduced from optically thick lines, A & A, 1981, 103: 160.[5] Fontenla, J. M., Avrett, E. H., Loeser, R., Energy balance in the solar transition region II. Effects of pressure and energy input on hydrostatic models, ApJ, 1991, 377: 712.[6] Fontenla, J. M., Avrett, E. H., Loeser, R., Energy balance in the solar transition region III. Helium emission in hydrostatic, constant-abundance models with diffusion, ApJ, 1993, 406: 319.[7] Pierce, A. K., Slaughter, C., Solar limb darkening I: λλ(30337297), Solar Phys., 1977, 51: 25.[8] Pierce, A. K., Slaughter, C., Weinberger, D., Solar limb darkening in the interval 740424018*!, II, Solar Phys., 1977, 52: 179.[9] Nechel, H., Labs, D., The solar radiation between 3300 and 12500*!, Solar Phys., 1984, 90: 205.[10] Vernazza, J. E., Avrett, E. H., Loeser, R., Structure of the solar chromosphere I. Basic computations and summary of the results, ApJ, 1973, 184: 605.[11] Mihalas, D., Stellar Atmospheres, San Francisco: W. H. Freeman and Company, 1978.[12] Fang, C., Hnoux, J. -C., Self-consistent model of flare heated solar chromosphere, A & A, 1983, 118: 139.[13] Ding, M. D., Fang, C., A semi-empirical model of sunspot penumbra, A & A, 1989, 225: 204.[14] Vernazza, J. E., Avrett, E. H., Loeser, R., Structure of the solar chromosphere III. Models of the EUV brightness components of the quiet Sun, ApJ Suppl., 1981, 45: 635.[15] Canfield, R. C., Athey, R

  6. Network and Plage Indices from Kodaikanal Ca-K Data

    CERN Document Server

    Raju, K P

    2013-01-01

    The Ca II K filtergrams from Kodaikanal Solar Observatory have been used to study the 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 declining activity period in both the indices. A comparison of network indices from the northern and the southern hemispheres shows that the former is more active than latter. However such an asymmetry is not clearly seen in the case of plage index.

  7. IRIS Observation of a Sunspot and the Surrounding Plage Region

    Science.gov (United States)

    TIAN, H.; DeLuca, E. E.; Mcintosh, S. W.; Reeves, K. K.; McKillop, S.; Weber, M.; Saar, S.; Golub, L.; Testa, P.

    2013-12-01

    NASA's IRIS mission is providing high-cadence and high-resolution observations of the solar transition region and chromosphere. We present preliminary results from IRIS observation of a sunspot and the surrounding plage region. The major findings in this observation can be summarized as following: (1) The slit jaw images in the filters of 1400Å and 1330Å reveal the presence of many rapidly evolving fibril-like structures in the transition region for the first time. These thin and long structures mainly reside in the plage region. They could be strands of low-lying cool transition region loops or the transition region counterpart of chromospheric spicules. (2) The C II and Mg II line profiles are almost Gaussian in the sunspot umbra and clearly exhibit a deep reversal at the line center in the plage region, suggesting a greatly reduced opacity in the sunspot atmosphere. (3) Bidirectional jets are frequently occurring mainly in the plage region immediately outside the sunspot throughout the observation. Triple or double Gaussian fit to the line profiles of Si IV suggests a velocity as high as 100 km/s. These velocity values are of the same order of the Alfven speed in the transition region. (4)Three-minute oscillation is clearly present in the sunspot umbra. The oscillation is identified in not only the slit jaw images of 2796Å, 1400Å and 1330Å, but also in spectra of the bright Mg II, C II and Si IV lines. Strong non-linearity is clearly seen in the intensity and Doppler shift oscillations. Interestingly, the obvious increase of the line width only occurs at the times of largest blue shift. The correlated change of the intensity and Doppler shift suggests an upward propagating magneto-acoustic shock wave.

  8. Association of mid-infrared solar plages with Calcium K line emissions and magnetic structures

    CERN Document Server

    Marcon, R; Melo, A M; Kudaka, A S; Tandberg-Hanssen, E

    2007-01-01

    Solar mid-IR observations in the 8-15 micrometer band continuum with moderate angular resolution (18 arcseconds) reveal the presence of bright structures surrounding sunspots. These plage-like features present good association with calcium CaII K1v plages and active region magnetograms. We describe a new optical setup with reflecting mirrors to produce solar images on the focal plane array of uncooled bolometers of a commercial camera preceded by germanium optics. First observations of a sunspot on September 11, 2006 show a mid-IR continuum plage exhibiting spatial distribution closely associated with CaII K1v line plage and magnetogram structures. The mid-IR continuum bright plage is about 140 K hotter than the neighboring photospheric regions, consistent with hot plasma confined by the magnetic spatial structures in and above the active region

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

    African Journals Online (AJOL)

    ﺮﯿﯿﺴﺘﻟا. ؛. ﻞﺣﺎﺴﻟا. ؛. ﺔﺤﺼﻟا . Résumé. Les rejets des déchets solides sur nos plages constituent une véritable plaie qui dégrade la beauté des paysages. Pour cela ...

  10. La crise des plages: pénurie de sédiments

    Directory of Open Access Journals (Sweden)

    Roland PASKOFF

    1998-12-01

    Full Text Available L'érosion des plages est un phénomène général dans le monde. Elle est essentiellement due à une pénurie en sable et en galets sur les côtes. Cette pénurie, qui a commencé à se manifester après la fin de la transgression postglaciaire, a été accentuée à l'époque contemporaine par des actions humaines, en particulier la construction de barrages sur les fleuves. L'élévation attendue du niveau de la mer aggravera probablement l'érosion des plages.

  11. What do iris observations of Mg II k tell us about the solar plage chromosphere?

    CERN Document Server

    Carlsson, Mats; De Pontieu, Bart

    2015-01-01

    We analyze observations from the Interface Region Imaging Spectrograph of the Mg II k line, the Mg II UV subordinate lines, and the O I 135.6 nm line to better understand the solar plage chromosphere. We also make comparisons with observations from the Swedish 1 m Solar Telescope of the H{\\alpha} line, the Ca II 8542 line, and Solar Dynamics Observatory/Atmospheric Imaging Assembly observations of the coronal 19.3 nm line. To understand the observed Mg II profiles, we compare these observations to the results of numerical experiments. The single-peaked or flat-topped Mg II k profiles found in plage imply a transition region at a high column mass and a hot and dense chromosphere of about 6500 K. This scenario is supported by the observed large-scale correlation between moss brightness and filled-in profiles with very little or absent self-reversal. The large wing width found in plage also implies a hot and dense chromosphere with a steep chromospheric temperature rise. The absence of emission in the Mg II subo...

  12. What Do IRIS Observations of Mg II k Tell Us about the Solar Plage Chromosphere?

    Science.gov (United States)

    Carlsson, Mats; Leenaarts, Jorrit; De Pontieu, Bart

    2015-08-01

    We analyze observations from the Interface Region Imaging Spectrograph of the Mg ii k line, the Mg ii UV subordinate lines, and the O i 135.6 {nm} line to better understand the solar plage chromosphere. We also make comparisons with observations from the Swedish 1-m Solar Telescope of the Hα line, the Ca ii 8542 line, and Solar Dynamics Observatory/Atmospheric Imaging Assembly observations of the coronal 19.3 {nm} line. To understand the observed Mg ii profiles, we compare these observations to the results of numerical experiments. The single-peaked or flat-topped Mg ii k profiles found in plage imply a transition region at a high column mass and a hot and dense chromosphere of about 6500 K. This scenario is supported by the observed large-scale correlation between moss brightness and filled-in profiles with very little or absent self-reversal. The large wing width found in plage also implies a hot and dense chromosphere with a steep chromospheric temperature rise. The absence of emission in the Mg ii subordinate lines constrain the chromospheric temperature and the height of the temperature rise while the width of the O i 135.6 {nm} line sets a limit to the non-thermal velocities to around 7 km s-1.

  13. La nouvelle Afrique du Sud à la plage ! Usages et fréquentation de trois plages de la péninsule du Cap

    Directory of Open Access Journals (Sweden)

    Hélène Frogneux

    2010-09-01

    Full Text Available Le Cap est souvent considéré comme étant la plus européenne des villes sud-africaines. Sa situation littorale a contribué à en faire à la fois un port majeur et une destination balnéaire prisée, tant par les Sud-Africains que par les visiteurs étrangers. Comme tous les espaces publics, les plages tombaient, sous l’apartheid, sous le coup des lois de ségrégations. Elles sont aujourd’hui théoriquement ouvertes à tous. Mais le décalage entre déségrégation institutionnelle et déségrégation dans les faits est important. Les plages capetoniennes donnent donc un aperçu des grandes tendances à l’œuvre en Afrique du Sud à l’aube de la Coupe du Monde 2010.According to all, Cape Town is the most European of South-African cities. Due to its coastal situation Cape Town is both a major port and an appreciated seaside destination, both by the South-Africans and by the foreign tourists. As was every public space, beaches were segregated under apartheid. Nowadays they are theoretically open to everyone, without distinction of race. But there is a gap between institutional desegregation and the desegregation de facto. Capetonian beaches reflect the mutations and the changes going on at the dawn of the 2010 World Cup.

  14. 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.

  15. 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.

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

    CERN Document Server

    Dumusque, X; Santos, N C

    2014-01-01

    This paper presents SOAP 2.0, a new version of the SOAP code that estimates in a simple way the photometric and radial velocity variations induced by active regions. The inhibition of the convective blueshift 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 convective blueshift 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 full width at half maximum (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 \\vsini$\\le8$\\kms. A ratio smaller than three implies a spot, while a larger ratio implies a plage. Using the observation of HD189733, we show that SOA...

  17. 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).

  18. 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.

  19. Long-term Variations in the Intensity of Plages and Networks as Observed in Kodaikanal Ca-K Digitized Data

    Science.gov (United States)

    Priyal, Muthu; Singh, Jagdev; Belur, Ravindra; Rathina, Somasundaram Kameshwaran

    2017-07-01

    In our previous article (Priyal et al. in Solar Phys. 289, 127, 2014) we have discussed the details of observations and methodology adopted to analyze the Ca-K spectroheliograms obtained at the Kodaikanal Observatory (KO) to study the variation of Ca-K plage areas, enhanced network (EN), and active network (AN) for Solar Cycles, namely 19, 20, and 21. Now, we have derived the areas of chromospheric features using KO Ca-K spectroheliograms to study the long-term variations of Solar Cycles 14 to 21. The comparison of the derived plage areas from the data obtained at the KO observatory for the period 1906 - 1985 with that of MWO, NSO for the period 1965 - 2002, earlier measurements made by Tlatov, Pevtsov, and Singh ( Solar Phys. 255, 239, 2009) for KO data, and the SIDC sunspot numbers shows a good correlation. The uniformity of the data obtained with the same instrument remaining with the same specifications provided a unique opportunity to study long-term intensity variations in plages and network regions. Therefore, we have investigated the variation of the intensity contrast of these features with time at a temporal resolution of six months assuming that the quiet-background chromosphere remains unchanged during the period 1906 - 2005 and found that the average intensity of the AN, representing the changes in small-scale activity over solar surface, varies with solar cycle being less during the minimum phase. In addition, the average intensity of plages and EN varies with a very long period having a maximum value during Solar Cycle 19, which was the strongest solar cycle of twentieth century.

  20. Developpement et application d'un systeme mobile de laser terrestre pour quantifier le bilan sedimentaire des plages

    Science.gov (United States)

    Van-Wierts, Stefanie

    Au Québec maritime, l'érosion côtière est une problématique d'envergure, notamment sur les côtes de formations meubles. Les plages ont un rôle de zone tampon ayant comme fonction naturelle d'absorber l'énergie des vagues et donc d'assurer l'équilibre de certains écosystèmes et le maintien de l'écoumène en réduisant l'érosion de la côte. Les méthodes d'acquisition conventionnelles ne permettent pas de quantifier convenablement les changements morphosédimentaires d'une plage à l'échelle des cellules hydrosédimentaires. Le manque de méthode d'acquisition fiable et de données quantitatives mène à une surestimation ou à une sous-estimation de la disponibilité sédimentaire d'un système côtier. Pour contrer ces lacunes et afin de minimiser les coûts d'acquisition, un nouveau système mobile de LiDAR terrestre a été mis en place, permettant d'acquérir des données topographiques de l'estran, de la haute plage et des falaises. Le système multicapteurs comprend un LiDAR, un système de navigation à haute précision (IMU et D-GPS) et une caméra. L'ensemble des instruments et capteurs sont montés sur un véhicule de type tout-terrain. Le système a été évalué sur la zone côtière de la péninsule de Manicouagan. La comparaison des données LiDAR avec 1 050 points de référence géopositionnés au D-GPS montre une erreur verticale moyenne de 0,1 m sur les secteurs de plage. Les résultats montrent que le volume sédimentaire moyen des plages devant les zones où la ligne de rivage présente un ouvrage de protection en enrochement (12 m 3/m) est plus de trois fois plus faible que devant les secteurs à l'état naturel (35,5 m3/m). La moyenne des secteurs en transition, constituant les segments où une zone artificielle et une zone naturelle se chevauchent présentent un volume moyen de 28 m3/m. Aussi, les plages devant les secteurs anthropisés sont en moyenne près de 2 fois plus étroites (12,7 m) que devant les secteurs naturels (25

  1. Modélisation de l’évolution des profils de plage sableuse sur plusieurs mois et apports de l’assimilation de données

    NARCIS (Netherlands)

    Dubarbier, B.; Castelle, B.; Birrien, F.; Marieu, V.; Ruessink, B.G.

    2012-01-01

    Dans ce papier nous présentons un nouveau modèle de profil de plage sableuse réalisant le couplage vagues/transport sédimentaire/évolution bathymétrique avec une approche à phase moyennée. Nous utilisons une paramétrisation récente des effets non-linéaires des vitesses orbitales des vagues au

  2. Mise au point d’und méthode d’isolement des Talitres (Crustacés Amphipodes) à partir des laisses de plage

    NARCIS (Netherlands)

    Ciavatti, Gérard

    1983-01-01

    Les Talitridés ( Orchestia platensis Kröyer, 1845) fuient les laisses de plage qui ont été inondées. La méthode d’isolement décrite exploite ce comportement. Elle permet d’isoler 97% des Talitres contenus dans les laisses. Elle pourrait être utilisée dans des études de biomasse et de productivité de

  3. 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)

  4. 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...

  5. Impact of occultations of stellar active regions on transmission spectra: Can occultation of a plage mimic the signature of a blue sky?

    CERN Document Server

    Oshagh, M; Ehrenreich, D; Haghighipour, N; Figueira, P; Santerne, A; Montalto, M

    2014-01-01

    Transmission spectroscopy during planetary transits, which is based on the measurements of the variations of planet-to-star radius ratio as a function of wavelength, is a powerful technique to study the atmospheric properties of transiting planets. One of the main limitation of this technique is the effects of stellar activity, which up until now, have been taken into account only by assessing the effect of non-occulted stellar spots on the estimates of planet-to-star radius ratio. In this paper, we study, for the first time, the impact of the occultation of a stellar spot and plage on the transmission spectra of transiting exoplanets. We simulated this effect by generating a large number of transit light curves for different transiting planets, stellar spectral types, and for different wavelengths. Results of our simulations indicate that the anomalies inside the transit light curve can lead to a significant underestimation or overestimation of the planet-to-star radius ratio as a function of wavelength. At ...

  6. 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 lot...

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

    CERN Document Server

    Flores-Soriano, Manuel

    2016-01-01

    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 H$\\alpha$ and H$\\beta$ lines, and the distribution of cool spots from Doppler maps. During our observations one side of the star was more active than the other. The equivalent width of the H$\\alpha$ line from the least active hemisphere increased from ~0.7 \\AA\\ at the beginning of the observation to 1.0 \\AA\\ at the end. The basal emission of the most active hemisphere remained roughly constant at a H$\\alpha$ EW of ~1.0 \\AA. Intense flare activity was observed during the first twenty days, where at least four different events were detected. The line asymmetries of the H$\\alpha$ line suggest that one of the flares could have produced a mass ejection with a maximum projected speed of $\\mathrm{70\\thinspace km\\thinspace s^{-1}}$. The rotational modulation of the V-band photometry showed clear anti-correlation with the chr...

  8. 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.

  9. 77 Restauration de plages nues d'une brousse tachetée au Niger ...

    African Journals Online (AJOL)

    AKA BOKO

    plantation d'espèces locales dans des ouvrages antiérosifs du type tranchées sylvopastorales. ... The effect of antierosive work on soil moisture was also ... du changement climatique, situation qui compromet la durabilité des systèmes de ..... 0,78 dans la zone-témoin, traduisant une distribution régulière de la régénération ...

  10. Evolutionary Charts of Solar Activity (Calcium Plages) as Functions of Heliographic Longitude and Time 1964-1979

    Science.gov (United States)

    1981-08-01

    Solar-Terrestrial Physics, Boulder, CO; Juan 0. Roederer, University of Denver, Denver, CO; and M.A. Shea and D.F. Smart, Air Force Cambridge Research...and Its Consequences for Data Acquisition, Documentation, Processing," by G.K. Hartmann, Mex-Planck-Institut fur Aeronomie, Lindau , GFR, May 1978, 36

  11. SURVIE DES BACTER I ES ISSUES D U REJET D’ABATTOIR DANS LES E A UX DE LA PLAGE D’EL JADIDA (MAROC

    Directory of Open Access Journals (Sweden)

    M. CHENNAOUI

    2013-02-01

    Full Text Available The present study on the survival of bacteria from the rejection of an abattoir in seawater was carried out in the laboratory and insitu. Abiotic factors studied in thelaboratory are solar radiation, temperature and salinity. To evaluate the effect of biotic and abiotic factors on the survival of bacteria in natural conditions, diffusion chamberswere used. The results highlight the importance of these stress parameters in the inactivation of bacteria. The percentages of dormancy can reach 98% to high salinity.The results of in situ tests show a reduction in bacterial numbers greater than during the study in the laboratory. The comparative study of counting techniques used shows that the abiotic and biotic factors have a bactericidal or bacteriostatic effect, which causesthe transformation of bacteria viable non-culturable state allowing them to retain their pathogenicity.

  12. LES RISQUES D’ÉROSION SUR LES RIVES DES ÉTANGS, LE CAS DU DÉMAIGRISSEMENT DES PLAGES

    Directory of Open Access Journals (Sweden)

    L. TOUCHART

    2012-12-01

    Full Text Available Ponds shore management and beach erosion risk. Ponds are very small water bodies where shore erosion mainly depends on wind waves. In Central-Western France (departments of Indre, Vienne, Haute-Vienne and Creuse some fifty ponds present artificial beaches for tourism. Maps of effective lengths and fetches allow to estimate the beach erosion hazard. The example of the Rochegaudon pond (municipality of Chaillac, which is an oblong pond from north to south with a crescent form, shows that the theoretical maximum erosion (effective length calculation occurs in the extremities and on the convex shore. The compass card of the meteorological station adds some information aboutsouth-western dominant winds. We suggest new morphoclimatic indicators such as asymmetric effective fetch and coefficiented fetch, whose computing and mapping show a maximum shore erosion in the north-east of the pond. This part of the shore just coincides with the beach of Rochegaudon, which took place on ancient micro-cliffs buried under a big artificial input of granitic sand. The choice of the beach location previously depended of criteria such as the nearness of the camping site, the road and the car park. At the present time the municipality manages the beach erosion by supplying every year the beach with sand.

  13. Analyse multi-échelle de la morphodynamique d'une plage artificielle, Avant-port Ouest de Dunkerque (Nord de la France).

    OpenAIRE

    Bertier, Jimmy

    2009-01-01

    Summary The Clipon beach is a13 km long artificial beach, created in the 1960s, following the extension of Dunkirk harbour. This study is based on a multiscale approach: a temporal scale extending from half a century to the tidal period, and a spatial scale going from the analysis of the morphological dynamics of the whole beach (104 m) to the examination of the morphosedimentary processes of elementary landforms like intertidal bars (101 - 102 m). The large-scale analysis concerns (1) coastl...

  14. Insulated DC-to-DC converter with wide input voltage range; Convertisseur continu-continu isole a large plage de tension d'entree: conception d'une alimentation 36 kW pour auxiliaire ferroviaire

    Energy Technology Data Exchange (ETDEWEB)

    Rieux, O.

    2000-11-15

    This thesis presents the research that has been carried out in the context of a collaboration contract between the FAIVELEY Transport company and the laboratoire d'Electrotechnique et d'Electronique Industrielle Laboratory. The goal of this research is the study of a converter that feeds a railway air conditioning unit, and that is fed by the overhead line voltage. It is an insulated DC-to-DC converter, of which input voltage varies from 2 to 5 kV, and output voltage is 600 V. This document introduces and justifies an original energy conversion principle. This principle is based on a series association of ZVS inverters, and a co-ordinated control that takes up the input voltage variations. This document also exposes detailed operation, and design rules applicable to converters based on this principle. Related studies are presented too, on such subjects as in situ reconnection of inverters for adapting to other overhead line types, or fault tolerance. Operation of such a converter has been studied by simulation, thus validating both the topology and the control modes. Experiments have also been carried out to check feasibility of a critical component of the structure: the saturable inductor. (author)

  15. A. Lambert, Protection durable du littoral varois : fonctionnement hydrosédimentaire de plages micro‑tidales équipées de systèmes de drainage

    OpenAIRE

    Héquette, Arnaud

    2007-01-01

    Les problèmes d’instabilité du trait de côte sont une préoccupation croissante le long de la plupart des littoraux du monde, particulièrement le long des côtes sableuses dont la majorité sont en érosion depuis plusieurs décennies. Le recul des côtes est d’autant plus inquiétant que l’occupation humaine de la frange côtière ne fait qu’augmenter, ce qui a conduit à développer diverses méthodes de lutte contre l’érosion allant de l’ouvrage d’art à des procédés dits « souples » qui présentent cha...

  16. 绝望与荒谬的抗争——关于阿尔贝·加缪《鼠疫》的解析%Struggle between Hopeless and Absurdity: Analysis of "The plage" by Albert Camus

    Institute of Scientific and Technical Information of China (English)

    刘小勤; 刘小燕

    2013-01-01

    加缪在小说《鼠疫》中虚构了一场突如其来的鼠疫袭击奥兰小城,给人们的社会生活带来巨大冲击,展现了死亡阴影笼罩下的恐怖乱象,作者集中塑造了以里厄医生为代表的、为挽救人类自身命运而进行的集体抗争行动,不仅体现了加缪对人类生存状况的高度关注,也凸显出人类应对一切荒谬现实、勇于抗争的理性、善良与勇敢的人文价值.%Albert Camus invented a precipitate plague which attacked Oran City and brought enormous impacts on human lives, revealing horrible chaos under the shadow of death.The author created a collective team, represented by Dr.Bernard Rieux, to struggle against human fate and save people's lives."The Plague" not only exhibited Albert Camus consistent focusing attention on human subsistence, but also prominent shows rational brave social and human values of human struggle against absurd reality during the battle against plague.

  17. 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.)

  18. 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)

  19. Mobilité du trait de côte en baie de Saint-Michel-en-Grève (Côtes d'Armor) ou le résultat d'une plage en accrétion

    OpenAIRE

    Stéphan, Pierre; Suanez, Serge

    2004-01-01

    International audience; Depuis plusieurs décennies, la baie de Saint-Michel-en-Grève connaît un engraissement sédimentaire important à l'origine de la progradation du trait de côte. A partir de ces observations, cette étude reprend l'ensemble de la question en privilégiant l'approche quantitative. Les résultats qui sont ici présentés reposent sur des mesures topo-morphologiques effectuées depuis 1998 et sur une étude de la cinématique du trait de côte par photo-interprétation.

  20. 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.)

  1. Optical and UV spectra of RS CVn stars

    Science.gov (United States)

    Ramsey, Lawrence W.

    1990-01-01

    The observed phenomenology in RS CVn and related binary systems is considered in terms of its modeling according to solar activity by examining UV and optical spectroscopy. Current data are examined to validate the existence of cool starspots, plage, prominences, and flares, as well as to determine the consistency of spatial correlations given by these data. RS CVn stars show spots at or near the poles, contrasting the low latitudes of solar spots; plage appears to be associated with cool spots on BY Draconis-like systems; plage and prominences, although identified as distinct phenomena, are theorized to be the same event in some cases. More spectroscopic and photometric observations are proposed to identify the detailed structure and locations of spots. UV and visible data are also required to distinguish plage regions from flare variations as well as determine the relation of extended structures to starspot and plage phenomena in RS CVn systems.

  2. Fragilisation et modification des formations littorales meubles sur l’île d’Anjouan (Comores) : Quand l’érosion d'origine anthropique se conjugue au changement climatique

    OpenAIRE

    Sinane, Kamardine; David, Gilbert; Pennober, Gwenaëlle; Troadec, Roland

    2011-01-01

    Sur l’île d’Anjouan, aux Comores, les premiers levés topographiques effectués sur les plages entre 2008 et 2009 montrent des morphotypes de profils à tendance convexe ou concave accusée. L’évolution de ces profils de plages est influencée par l’extraction du sable et par l’exposition aux forçages météo-marins. L’extraction du sable de plage est plus importante sur les plages avec des profils concaves accusés que celles avec des profils à tendance convexe. L’érosion qui en résulte est souvent...

  3. 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.

  4. Butterfly Diagram and Carrington Maps for Century-Long Ca II K Spectroheliograms from Kodaikanal Observatory

    CERN Document Server

    Chatterjee, Subhamoy; Ravindra, B

    2016-01-01

    The century-long (1907-2007) Ca II K spectroheliograms from Kodaikanal Solar Observatory (KSO) are calibrated, processed and analysed in the present study to follow the evolution of bright on disc structures called plages, the possible representatives of magnetic activity on the Sun. This has been the longest dataset studied in Ca II K till date covering about 9.5 cycles of 11 year periods. Plages were segmented with area $\\geq 1\\:\\textrm {arcmin}^2$ using global thresholds for individual full disc images and subsequent application of morphological closing operation. Plage index was calculated and seen to have close positive correlation with fractional disc area covered by plages. The newly generated plage area cycle (from KSO) was compared with the same from Mount Wilson observatory (Correlation~$95.6\\%$) for the overlapping years i.e. 1915-2000. Study illustrated time-latitude distribution of plage centroids rendering butterfly diagram (as observed for sunspots). The 3D visualisation of the diagram showed o...

  5. Fourier transform spectrometer observations of solar carbon monoxide. II - Simultaneous cospatial measurements of the fundamental and first-overtone bands, and Ca II K, in quiet and active regions

    Science.gov (United States)

    Ayres, T. R.; Testerman, L.; Brault, J. W.

    1986-01-01

    Fourier transform spectrometry has yielded simultaneous cospatial measurements of important diagnostics of thermal structure in the high solar photosphere and low chromosphere. It is noted that the anomalous behavior of the fundamental bands of CO in quiet areas near the limb is accentuated in an active region plage observed close to the limb. The difference between the core temperatures of the CO fundamental bands in a plage and a nearby quiet region at the limb is larger than the corresponding brightness temperature differences in the inner wings of the Ca II line measured in a quiet region and several plages closer to the disk center. Numerical simulations indicate that the disparate behavior of the CO bands with respect to Ca II K cannot be reconciled with existing single component thermal structure models; a two-component atmosphere is required.

  6. The dark side of solar photospheric G-band bright points

    Science.gov (United States)

    Riethmüller, T. L.; Solanki, S. K.

    2017-02-01

    Bright, small-scale magnetic elements found mainly in intergranular lanes at the solar surface are named bright points (BPs). They show high contrasts in Fraunhofer G-band observations and are described by nearly vertical slender flux tubes or sheets. A recent comparison between BP observations in the ultraviolet (UV) and visible spectral range recorded with the balloon-borne observatory Sunrise and state-of-the-art magnetohydrodynamical (MHD) simulations revealed a kilogauss magnetic field for 98% of the synthetic BPs. Here we address the opposite question, namely which fraction of pixels hosting kilogauss fields coincides with an enhanced G-band brightness. We carried out 3D radiation MHD simulations for three magnetic activity levels (corresponding to the quiet Sun, weak and strong plage) and performed a full spectral line synthesis in the G-band. Only 7% of the kilogauss pixels in our quiet-Sun simulation coincide with a brightness lower than the mean quiet-Sun intensity, while 23% of the pixels in the weak-plage simulation and even 49% in the strong-plage simulation are associated with a local darkening. Dark strong-field regions are preferentially found in the cores of larger flux patches that are rare in the quiet Sun, but more common in plage regions, often in the vertices of granulation cells. The significant brightness shortfall in the core of larger flux patches coincides with a slight magnetic field weakening. Kilogauss elements in the quiet Sun are, on average, brighter than similar features in plage regions. Almost all strong-field pixels display a more or less vertical magnetic field orientation. Hence, in the quiet Sun, G-band BPs correspond almost one-to-one with kilogauss elements. In weak plage, the correspondence is still very good, but not perfect.

  7. 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.)

  8. 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.

  9. Verteringsenzymen van insecten als doel voor plantaardige afweerstoffen

    NARCIS (Netherlands)

    Beekwilder, M.J.

    2003-01-01

    De verteringsenzymen (proteases) van insecten zijn een doel waarop planten hun afweer richten. Die afweer bestaat uit het produceren van proteaseremmers, die de proteases in de insectendarm blokkeren. Deze manier van bescherming kan ook via genetische modificatie in planten ingebouwd worden om plage

  10. Solar transition region above sunspots

    CERN Document Server

    Tian, H; Teriaca, L; Landi, E; Marsch, E

    2009-01-01

    We study the TR properties above sunspots and the surrounding plage regions, by analyzing several sunspot spectra obtained by SUMER in March 1999 and November 2006. We compare the SUMER spectra observed in the umbra, penumbra, plage, and sunspot plume regions. The Lyman line profiles averaged in each region are presented. For the sunspot observed in 2006, the electron densities, DEM, and filling factors of the TR plasma in the four regions are also investigated. The self-reversals of the Lyman line profiles are almost absent in umbral regions at different locations (heliocentric angle up to $49^\\circ$) on the solar disk. In the sunspot plume, the Lyman lines are also not reversed, whilst the lower Lyman line profiles observed in the plage region are obviously reversed. The TR densities of the umbra and plume are similar and one order of magnitude lower than those of the plage and penumbra. The DEM curve of the sunspot plume exhibits a peak centered around $\\log(T/\\rm{K})\\sim5.45$, which exceeds the DEM of oth...

  11. Correlation of noise storm and H-alpha activity for the CONS period Sept. 1 - 4, 1980.

    Science.gov (United States)

    Vršnak, B.; Ruždjak, V.

    The Ca plage index was found to be highly correlated with the 260 MHz radio flux. The noise storm enhancement followed the increase in the number of major flares with the delay of one day. The noise storm behaviour was correlated with the three hour flare index, but not with the one hour flare index.

  12. The Variability of Solar Spectral Irradiance and Solar Surface Indices Through the Solar Activity Cycles 21-23

    Science.gov (United States)

    Deniz Goker, Umit

    2016-07-01

    A study of variations of solar spectral irradiance (SSI) in the wavelength 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 as SME (NSSDC), UARS (GDAAC), SORCE (LISIRD) and SIDC, respectively. We developed a special software for extracting the data and reduced this data by using the MATLAB. In this respect, we revealed negative correlations of intensities of UV (289.5 nm-300.5 nm) emission lines originating in the solar chromosphere with the ISSN index during the unusually prolonged minimum between the solar cycles (SCs) 23 and 24. We also compared our results with the ground-based telescopes as Solar Irradiance Platform, Stanford Data (SFO), Kodaikanal Data (KKL) and NGDC Homepage (Rome and Learmonth Solar Observatories). We studied the variations of total solar irradiance (TSI), magnetic field, sunspots/sunspot groups, Ca II K-flux, faculae and plage areas data with these ground-based telescopes, respectively. We reduced the selected data using the Phyton programming language and plot with the IDL programme. Therefore, we found that there was a decrease in the area of bright faculae and chromospheric plages while the percentage of dark faculae and plage decrease, as well. However, these decreases mainly occurred in small sunspots, contrary to this, these terms in large sunspot groups were comparable to previous SCs or even larger. Nevertheless, negative correlations between ISSN and SSI data indicate that these emissions are in close connection with the classes of sunspots/sunspot groups and "PLAGE" regions. Finally, we applied the time series of the chemical elements correspond to the wavelengths 121.5 nm-300.5 nm and compared with the ISSN data. We found an unexpected increasing in the 298.5 nm for the Fe II element. The variability of Fe II (298.5 nm) is in close connection with the plage regions and the sizes of the

  13. Solar Spectral Irradiance Variability of Some Chromospheric Emission Lines Through the Solar Activity Cycles 21-23

    Science.gov (United States)

    Göker, Ü. D.; Gigolashvili, M. Sh.; Kapanadze, N.

    2017-02-01

    A study of variations of solar spectral irradiance (SSI) in the wavelength 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 MATLAB software 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.

  14. Long Term Variations in Chromospheric Features from Ca-K Images at Kodaikanal

    Science.gov (United States)

    Priyal, Muthu; Singh, Jagdev; Ravindra, B.; Priya, T. G.; Amareswari, K.

    2014-01-01

    There is a collection of about 100 years of Ca-K line spectroheliograms at the Kodaikanal Observatory (KKL) obtained on daily basis with a single instrument that can be used to study long term variations of various chromospheric features. All the Ca-K images have been digitized using specially developed digitizers with uniform and highly stable light source, high quality lens and 4k×4k format CCD camera. The digitization has been carried out in a room with controlled temperature and humidity. The digitized data are in 16-bit format with pixel resolution of 0.86 arcsec. The digitized images have been calibrated by a process that includes flat-fielding, density to intensity conversion, centering the image, and rotation of the image to make the solar north pole in the fixed direction. Then we applied correction for the limb darkening effect and also made the background in the image uniform. The image background was normalized to unity that enabled us to use the intensity contrast to identify different features, such as plages, enhanced (EN), active (AN), and quite network on images and classified them by using different image contrast and area threshold values. After several experiments with different threshold values for different features and careful analysis of a large number of images, we could fix the threshold values of intensity contrast larger than 1.35 and area larger than 1 arcmin2 for plages, larger than 1.35 but area less than 1 arcmin2 for EN, and between 1.25 - 1.35 for AN. We compared the quarterly averaged and half yearly averaged plage areas obtained from KKL with the Mount Wilson (MWO) data and sunspot number. We find that the plage area extracted from the KKL is highly correlated with the MWO plage area, though there is a slight difference between the two data set in cycle 19. The plage area of KKL is also highly correlated with the sunspot number. The areas of EN and AN are also found to have smaller quasi-periodic variations apart from the solar

  15. A Century of Solar Ca ii Measurements and Their Implication for Solar UV Driving of Climate

    Science.gov (United States)

    Foukal, Peter; Bertello, Luca; Livingston, William C.; Pevtsov, Alexei A.; Singh, Jagdev; Tlatov, Andrey G.; Ulrich, Roger K.

    2009-04-01

    Spectroheliograms and disk-integrated flux monitoring in the strong resonance line of Ca ii (K line) provide the longest record of chromospheric magnetic plages. We compare recent reductions of the Ca ii K spectroheliograms obtained since 1907 at the Kodaikanal, Mt. Wilson, and US National Solar Observatories. Certain differences between the individual plage indices appear to be caused mainly by differences in the spectral passbands used. Our main finding is that the indices show remarkably consistent behavior on the multidecadal time scales of greatest interest to global warming studies. The reconstruction of solar ultraviolet flux variation from these indices differs significantly from the 20th-century global temperature record. This difference is consistent with other findings that, although solar UV irradiance variation may affect climate through influence on precipitation and storm tracks, its significance in global temperature remains elusive.

  16. A chromospheric conundrum?

    CERN Document Server

    Judge, Philip; Schmidt, Wolgang; Steiner, Oskar

    2010-01-01

    We examine spectra of the Ca II H line, obtained under good seeing conditions with the VTT Echelle Spectrograph in June of 2007, and higher resolution data of the Ca II 8542 Angstrom line from Fabry-Perot instruments. The VTT targets were areas near disk center which included quiet Sun and some dispersed plage. The infrared data included quiet Sun and plage associated with small pores. Bright chromospheric network emission patches expand little with wavelength from line wing to line center, i.e. with increasing line opacity and height. We argue that this simple observation has implications for the force and energy balance of the chromosphere, since bright chromospheric network emission is traditionally associated with enhanced local mechanical heating which increases temperatures and pressures. Simple physical considerations then suggest that the network chromosphere may not be able to reach horizontal force balance with its surroundings, yet the network is a long-lived structure. We speculate on possible rea...

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

    CERN Document Server

    Jain, Rekha; 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 supression in plage and magnetic elements, by modelling 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 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 wit...

  18. Radiative emission of solar features in Ca II K

    CERN Document Server

    Criscuoli, S; Fontenla, J; Giorgi, F; Rast, M; Solanki, S; Uitenbroek, H

    2010-01-01

    We investigated the radiative emission of different types of solar features in the spectral range of the Ca II K line. We analyzed full-disk 2k x 2k observations from the PSPT Precision Solar Photometric Telescope. The data were obtained by using three narrow-band interference filters that sample the Ca II K line with different pass bands. Two filters are centered in the line core, the other in the red wing of the line. We measured the intensity and contrast of various solar features, specifically quiet Sun (inter-network), network, enhanced network, plage, and bright plage (facula) regions. Moreover, we compared the results obtained with those derived from the numerical synthesis performed for the three PSPT filters with a widely used radiative code on a set of reference semi-empirical atmosphere models.

  19. Detection of coherent structures in photospheric turbulent flows

    Energy Technology Data Exchange (ETDEWEB)

    Chian, Abraham C.-L.; Rempel, Erico L. [National Institute for Space Research (INPE), World Institute for Space Environment Research (WISER), P.O. Box 515, 12227-010 São José dos Campos-SP (Brazil); Aulanier, Guillaume; Schmieder, Brigitte [Observatoire de Paris, LESIA, CNRS, F-92190 Meudon (France); Shadden, Shawn C. [Department of Mechanical Engineering, University of California, Berkeley, CA 94720 (United States); Welsch, Brian T. [Space Science Laboratory, University of California, Berkeley, CA 94720 (United States); Yeates, Anthony R., E-mail: abraham.chian@gmail.com, E-mail: rempel@ita.br [Department of Mathematical Sciences, Durham University, Durham DH1 3LE (United Kingdom)

    2014-05-01

    We study coherent structures in solar photospheric flows in a plage in the vicinity of the active region AR 10930 using the horizontal velocity data derived from Hinode/Solar Optical Telescope magnetograms. Eulerian and Lagrangian coherent structures (LCSs) are detected by computing the Q-criterion and the finite-time Lyapunov exponents of the velocity field, respectively. Our analysis indicates that, on average, the deformation Eulerian coherent structures dominate over the vortical Eulerian coherent structures in the plage region. We demonstrate the correspondence of the network of high magnetic flux concentration to the attracting Lagrangian coherent structures (aLCSs) in the photospheric velocity based on both observations and numerical simulations. In addition, the computation of aLCS provides a measure of the local rate of contraction/expansion of the flow.

  20. Zoonosis Facts

    OpenAIRE

    1999-01-01

    Zoonosis is de ned as “an infectious disease transmissible under natural conditions between vertebrate animals and human beings” (Mast 95). There are more than 150 diseases recognized under the umbrella of zoonosis. Some of the better known examples include: anthrax, bursilosis, hunta virus, bubonic plage, hemoragic fevers like ebola, rabies, and even AIDS. The world’s most signi cant epidemic (the 1919 pandemic) was believed to have originated in swine near Fort Riley Kansas in 1917. This in...

  1. Mauritius An Oasis of Peace and Tranquility

    Institute of Scientific and Technical Information of China (English)

    2007-01-01

    @@ As Mark Twain noted of Mauritius in Following the Equator, "You gather the idea that Mauritius was made first and then heaven, and that heaven was copied after Mauritius." For those looking for the ultimate in exotic locations, Mauritius could be it. Mauritius continues to fulfill every visitor's dream of a tropical island, from swaying palms to the dazzling blue of the ocean - Ile aux Cerfs, at bottom left, Belle Mare plage on the right, balmy nights and smiling people………

  2. Determination of the chromospheric quiet network element area index and its variation between 2008 and 2011

    Institute of Scientific and Technical Information of China (English)

    Jagdev Singh; Ravindra Belur; Selvendran Raju; Kumaravel Pichaimani; Muthu Priyal; Thambaje Gopalan Priya; Amareswari Kotikalapudi

    2012-01-01

    In general,it is believed that plages and sunspots are the main contributors to solar irradiance.There are small-scale structures on the Sun with intermediate magnetic fields that could also contribute to solar irradiance,but it has not yet been quantified how many of these small scale structures contribute and how much this varies over the solar cycle.We used Ca Ⅱ K images obtained from the telescope at the Kodaikanal observatory.We report a method to separate the network elements from the background structure and plage regions,and compute the changes in the network element area index during the minimum phase of the solar cycle and part of the ascending phase of cycle 24.The measured area occupied by the network elements is about 30% and the plages cover less than 1% of the solar disk during the observation period from February 2008 to 2011.During the extended period of minimum activity,it is observed that the network element area index decreases by about 7% compared to the area occupied by the network elements in 2008.A long term study of the network element area index is required to understand the variations over the solar cycle.

  3. Solar Magnetoconvection and Small-Scale Dynamo. Recent Developments in Observation and Simulation

    Science.gov (United States)

    Borrero, J. M.; Jafarzadeh, S.; Schüssler, M.; Solanki, S. K.

    2017-09-01

    A number of observational and theoretical aspects of solar magnetoconvection are considered in this review. We discuss recent developments in our understanding of the small-scale structure of the magnetic field on the solar surface and its interaction with convective flows, which is at the centre of current research. Topics range from plage areas in active regions over the magnetic network shaped by supergranulation to the ubiquituous `turbulent' internetwork fields. On the theoretical side, we focus upon magnetic field generation by small-scale dynamo action.

  4. Synthèse de lois de commande non-linéaires pour un entrainement électrique à vitesse variable basé sur un moteur synchrone à aimants permanents

    OpenAIRE

    AID, Houssem; AINA, Wafaa

    2014-01-01

    Les moteurs synchrones à aimants permanents sont de plus en plus utilisés dans les servomécanismes grâce à leurs performances supérieures aux autres moteurs à courants alternatifs. Ce mémoire porte sur la commande à hautes performances du moteur synchrone à aimants permanents. Nous proposons la commande de la machine synchrone à aimants permanents avec orientation du flux rotorique. Cette commande consiste à éliminer le problème de cou-plage entre le flux et le couple en dissoc...

  5. Evidence for siphon flows with shocks in solar magnetic flux tubes

    Science.gov (United States)

    Degenhardt, D.; Solanki, S. K.; Montesinos, B.; Thomas, J. H.

    1993-01-01

    We synthesize profiles of the infrared line Fe I 15648.5 A (g = 3) for a recently developed theoretical model of siphon flows along photospheric magnetic loops. The synthesized line profiles are compared with the observations from which Rueedi et al. (1992) deduced the presence of such flows across the neutral line of an active region plage. This comparison supports the interpretation of Rueedi et al. (1992). It also suggests that the average footpoint separation of the observed loops carrying the siphon flow is 8-15 sec and that the siphon flow experiences a standing tube shock in the downstream leg near the top of the arch.

  6. Chapitre 13. L’impact macro-économique du narcotrafic en Colombie

    OpenAIRE

    2014-01-01

    Note portant sur l’auteur Un regard sur la carte du continent latino-américain permet de comprendre pourquoi la Colombie est au carrefour des routes de la cocaïne : elle est équidistante des champs de coca du Pérou et de Bolivie, et des plages de Floride. Son relatif développement industriel et commercial a permis aux institutions et aux individus d’acquérir les compétences requises, concernant la chimie du raffinage, les circuits de financement, et l’organisation du transport de la drogue. A...

  7. Apports des hautes résolutions spatiales pour l'étude et la cartographie des algues vertes. Application à la grève de St-Michel(22)

    OpenAIRE

    Ruiz, Olivier

    1994-01-01

    Les apports croissants d'effluents agricoles associés avec des situations hydrodynamiques particulières sont à l'origine de fortes proliférations d'algues vertes du type ulva lactuca (ulves). Lorsque la mer se retire les algues se déposent sur les plages et créent des nuisances pour le tourisme et les professionnels de la mer. Les estimations de biomasse sont alors nécessaires à la fois pour comprendre le phénomène et pour mesurer son ampleur. Pendant la période de forts coefficients de marée...

  8. Érosion marine, les réponses

    Directory of Open Access Journals (Sweden)

    Alain MIOSSEC

    1998-12-01

    Full Text Available Divers types de solution existent pour lutter contre l'érosion marine. Les moyens techniques ont eu, de longue date, la préférence des hommes. Les ouvrages de défense (digues, enrochements, épis et brise-lames sont généralement efficaces, mais perturbent l'équilibre morphodynamique des littoraux. D'autres méthodes, comme le rechargement des plages en sédiments, sont possibles. Il convient aussi de penser à de nouvelles réglementations des domaines hydrologiques.

  9. Les Cocotiers de la France : tourismes en Outre-mer

    Directory of Open Access Journals (Sweden)

    2010-02-01

    Full Text Available Diversité des territoires ultramarins, diversité des formes de tourisme.Au-delà du mythe océanien qui assimile cocotiers, soleil, plages de sable blanc et farniente, Jean-Christophe Gay étudie la production de ces espaces touristiques et met en évidence le faible développement de ce secteur d’activité, au regard des atouts et des investissements dont bénéficient globalement les territoires d’outremer.Son ouvrage se compose de trois grands chapitres :le tourisme ultramarin d’hier à aujourd’hui...

  10. On the triggering of a spotless double-ribbon flare

    Science.gov (United States)

    Rausaria, R. R.; Aleem, S. M.; Sundara Raman, K.

    1992-11-01

    We have studied the evolution of the double-ribbon, spotless flare of 21 February, 1992, using Kodaikanal H-alpha and Kfl observations. The analysis of the data shows that the H-alpha filament underwent a large change in shear prior to the day of the onset of the flare. We find considerable rotation of the plage region before the emergence of a small magnetic pore. It is concluded that shear plays an important role in the triggering of a spotless flare.

  11. Investigation of possible sun-weather relationships

    Energy Technology Data Exchange (ETDEWEB)

    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.

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

    Science.gov (United States)

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

    2017-08-01

    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 rad is observed, the slope is mean T B (1.25 mm) and mean T 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 rad 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.

  13. 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...

  14. 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.

  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. THE UBIQUITOUS PRESENCE OF LOOPLIKE FINE STRUCTURE INSIDE SOLAR ACTIVE REGIONS

    Energy Technology Data Exchange (ETDEWEB)

    Wang, Y.-M., E-mail: yi.wang@nrl.navy.mil [Space Science Division, Naval Research Laboratory, Washington, DC 20375 (United States)

    2016-03-20

    Although most of the solar surface outside active regions (ARs) is pervaded by small-scale fields of mixed polarity, this magnetic “carpet” or “junkyard” is thought to be largely absent inside AR plages and strong network. However, using extreme-ultraviolet images and line-of-sight magnetograms from the Solar Dynamics Observatory, we find that unipolar flux concentrations, both inside and outside ARs, often have small, loop-shaped Fe ix 17.1 and Fe xii 19.3 nm features embedded within them, even though no minority-polarity flux is visible in the corresponding magnetograms. Such looplike structures, characterized by horizontal sizes of ∼3–5 Mm and varying on timescales of minutes or less, are seen inside bright 17.1 nm moss, as well as in fainter moss-like regions associated with weaker network outside ARs. We also note a tendency for bright coronal loops to show compact, looplike features at their footpoints. Based on these observations, we suggest that present-day magnetograms may be substantially underrepresenting the amount of minority-polarity flux inside plages and strong network, and that reconnection between small bipoles and the overlying large-scale field could be a major source of coronal heating both in ARs and in the quiet Sun.

  17. A Statistical Analysis of Solar Surface Indices Through the Solar Activity Cycles 21-23

    CERN Document Server

    Goker, Umit Deniz; Nutku, Ferhat; Priyal, Muthu

    2016-01-01

    Variations of total solar irradiance (TSI), magnetic field, Ca II K-flux, faculae and plage areas due to the number and the type of sunspots/sunspot groups (SGs) are well established by using ground based data from various centers such as Solar Irradiance Platform, Stanford Data (SFO), Kodaikanal data (KKL) and National Geographical Data Center (NGDC) Homepage, respectively. We applied time series analysis for extracting the data over the descending phases of solar activity cycles (SACs) 21, 22 and 23, and the ascending phases 22 and 23 of SACs, and analyzed the selected data using the Python programming language. Our detailed analysis results suggest that there is a stronger correlation between solar surface indices and the changes in the relative portion of the small and large SGs. This somewhat unexpected finding suggest that plage regions decreased in a lower values in spite of the higher number of large SGs in SAC 23 while Ca II K-flux did not decrease by large amount or it was comparable with SAC 22 for...

  18. 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.

  19. 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.

  20. 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...

  1. SUMER-Hinode observations of microflares: excitation of molecular hydrogen

    CERN Document Server

    Innes, D E

    2007-01-01

    Concentrations of molecular hydrogen (H2) have been detected by SUMER in active region plage. The H2 is excited by O VI line emission at 1031.94 A which, although not observed, must be brightening along with the observed transition region line, Si III 1113.24 A. We have made co-ordinated observations of active region plage with the spectrometer SUMER/SoHO in lines of H2 1119.10 A and Si III 1113.24 A and with XRT/Hinode X-ray and SOT/Hinode Ca II filters. In six hours of observation, six of the seven H2 events seen occurred near a footpoint of a brightening X-ray loop. The seventh is associated with an unusually strong Si III plasma outflow. We conclude that microflare energy dissipation heats the chromosphere, reducing its opacity, so that O VI microflare emission is able to reach the lower layers of the chromosphere and excite the H2.

  2. Turbulent Diffusion in the Photosphere as Derived from Photospheric Bright Point Motion

    CERN Document Server

    Abramenko, V I; Yurchyshyn, V; Goode, P R; Stein, R F; Lepreti, F; Capparelli, V; Vecchio, A

    2011-01-01

    On the basis of observations of solar granulation obtained with the New Solar Telescope (NST) of Big Bear Solar Observatory, we explored proper motion of bright points (BPs) in a quiet sun area, a coronal hole, and an active region plage. We automatically detected and traced bright points (BPs) and derived their mean-squared displacements as a function of time (starting from the appearance of each BP) for all available time intervals. In all three magnetic environments, we found the presence of a super-diffusion regime, which is the most pronounced inside the time interval of 10-300 seconds. Super-diffusion, measured via the spectral index, $\\gamma$, which is the slope of the mean-squared displacement spectrum, increases from the plage area ($\\gamma=1.48$) to the quiet sun area ($\\gamma=1.53$) to the coronal hole ($\\gamma=1.67$). We also found that the coefficient of turbulent diffusion changes in direct proportion to both temporal and spatial scales. For the minimum spatial scale (22 km) and minimum time sca...

  3. 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.

  4. Radiative emission of solar features in the Ca II K line: comparison of measurements and models

    CERN Document Server

    Ermolli, I; Uitenbroek, H; Giorgi, F; Rast, M P; Solanki, S K

    2010-01-01

    We study the radiative emission of various types of solar features, such as quiet Sun, enhanced network, plage, and bright plage regions, identified on filtergrams taken in the Ca II K line. We analysed fulldisk images obtained with the PSPT, by using three interference filters that sample the Ca II K line with different bandpasses. We studied the dependence of the radiative emission of disk features on the filter bandpass. We also performed a NLTE spectral synthesis of the Ca II K line integrated over the bandpass of PSPT filters. The synthesis was carried out by utilizing both the PRD and CRD with the most recent set of semi­empirical atmosphere models in the literature and some earlier atmosphere models. We measured the CLV of intensity values for various solar features identified on PSPT images and compared the results obtained with those derived from the synthesis. We find that CRD calculations derived using the most recent quiet Sun model, on average, reproduce the measured values of the quiet Sun regi...

  5. Beyond sunspots: Studies using the McIntosh Archive of global solar magnetic field patterns

    Science.gov (United States)

    Gibson, Sarah E.; Webb, David; Hewins, Ian M.; McFadden, Robert H.; Emery, Barbara A.; Denig, William; McIntosh, Patrick S.

    2017-10-01

    In 1964 (Solar Cycle 20; SC 20), Patrick McIntosh began creating hand-drawn synoptic maps of solar magnetic features, based on Hα images. These synoptic maps were unique in that they traced magnetic polarity inversion lines, and connected widely separated filaments, fibril patterns, and plage corridors to reveal the large-scale organization of the solar magnetic field. Coronal hole boundaries were later added to the maps, which were produced, more or less continuously, into 2009 (i.e., the start of SC 24). The result was a record of ~45 years (~570 Carrington rotations), or nearly four complete solar cycles of synoptic maps. We are currently scanning, digitizing and archiving these maps, with the final, searchable versions publicly available at NOAA's National Centers for Environmental Information. In this paper we present preliminary scientific studies using the archived maps from SC 23. We show the global evolution of closed magnetic structures (e.g., sunspots, plage, and filaments) in relation to open magnetic structures (e.g., coronal holes), and examine how both relate to the shifting patterns of large-scale positive and negative polarity regions.

  6. 13CO mapping study for massive molecular cloud cores

    Institute of Scientific and Technical Information of China (English)

    WU; Yuefang

    2001-01-01

    [1] Zirin, H., Astrophysics of the Sun, Chapter 7, Cambridge: Cambridge University Press, 1988.[2] Shine, R. A., Linsky, J. L., Physical properties of solar chromospheric plages II. Chromospheric plage models, Solar Phys., 1974, 39: 49.[3] Kelch, W. L., Linsky, J. L., Physical properties of solar chromospheric plages III. Models based on CaII and MgII observations, Solar Phys., 1978, 58: 37.[4] Lemaire, P., Goutlebroze, J. C., Vial, J. C. et al., Physical properties of the solar chromosphere deduced from optically thick lines, A & A, 1981, 103: 160.[5] Fontenla, J. M., Avrett, E. H., Loeser, R., Energy balance in the solar transition region II. Effects of pressure and energy input on hydrostatic models, ApJ, 1991, 377: 712.[6] Fontenla, J. M., Avrett, E. H., Loeser, R., Energy balance in the solar transition region III. Helium emission in hydrostatic, constant-abundance models with diffusion, ApJ, 1993, 406: 319.[7] Pierce, A. K., Slaughter, C., Solar limb darkening I: λλ(30337297), Solar Phys., 1977, 51: 25.[8] Pierce, A. K., Slaughter, C., Weinberger, D., Solar limb darkening in the interval 740424018*!, II, Solar Phys., 1977, 52: 179.[9] Nechel, H., Labs, D., The solar radiation between 3300 and 12500*!, Solar Phys., 1984, 90: 205.[10] Vernazza, J. E., Avrett, E. H., Loeser, R., Structure of the solar chromosphere I. Basic computations and summary of the results, ApJ, 1973, 184: 605.[11] Mihalas, D., Stellar Atmospheres, San Francisco: W. H. Freeman and Company, 1978.[12] Fang, C., Hnoux, J. -C., Self-consistent model of flare heated solar chromosphere, A & A, 1983, 118: 139.[13] Ding, M. D., Fang, C., A semi-empirical model of sunspot penumbra, A & A, 1989, 225: 204.[14] Vernazza, J. E., Avrett, E. H., Loeser, R., Structure of the solar chromosphere III. Models of the EUV brightness components of the quiet Sun, ApJ Suppl., 1981, 45: 635.[15] Canfield, R. C., Athey, R

  7. Time-dependent suppression of oscillatory power in evolving solar magnetic fields

    CERN Document Server

    Prasad, S Krishna; Jain, R; Keys, P H

    2016-01-01

    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 powermaps, 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 utilising 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~\\textsc{ii}~K and H$\\alpha$ 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 ...

  8. Spatially Resolved Images and Solar Irradiance Variability

    Indian Academy of Sciences (India)

    R. Kariyappa

    2008-03-01

    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 magnetic activities that can be identified through spatially resolved photospheric, chromospheric and coronal features. In this research, the images of CaII K-line (NSO/Sac Peak) have been analysed to segregate the various chromospheric features.We derived the different indices and estimated their contribution from the time series data to total CaII K emission flux and UV irradiance variability. A part of the important results from this research is discussed in this paper.

  9. HARPS-N observes the Sun as a star

    CERN Document Server

    Dumusque, Xavier; Phillips, David F; Buchschacher, Nicolas; Cameron, Andrew Collier; Cecconi, Massimo; Charbonneau, David; Cosentino, Rosario; Ghedina, Adriano; Latham, David W; Li, Chih-Hao; Lodi, Marcello; Lovis, Christophe; Molinari, Emilio; Pepe, Francesco; Udry, Stephane; Sasselov, Dimitar; Szentgyorgyi, Andrew; Walsworth, Ronald

    2015-01-01

    Radial velocity 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 radial velocity changes. Over seven days of observing in 2014, we show an average 50\\cms radial velocity rms over a few hours of observation. After correcting observed radial velocities for spot and...

  10. Budget sédimentaire du littoral de la baie d’El Jadida (Maroc).

    OpenAIRE

    Chaïbi, Mohamed; Sabatier, François

    2011-01-01

    Plusieurs méthodes ont été utilisées pour calculer le budget sédimentaire de la baie d’El Jadida sur la côte Atlantique marocaine. Cet espace correspond partiellement à une plage urbaine et possède un fort potentiel touristique. L’étude montre un bilan sédimentaire globalement stable mais une zone centrale en érosion. Ce secteur affiche la plus forte vulnérabilité. L’oued Oum Er-Rbia, équipé de barrages depuis la fin des années 1940, ne fournit pas de sédiments à la zone de manière significat...

  11. The Solar Dynamo Zoo

    Science.gov (United States)

    Egeland, Ricky; Soon, Willie H.; Baliunas, Sallie L.; Hall, Jeffrey C.; Pevtsov, Alexei A.; Henry, Gregory W.

    2016-05-01

    We present composite time series of Ca II H & K line core emission indices of up to 50 years in length for a set of 27 solar-analog stars (spectral types G0-G5; within ~10% of the solar mass) and the Sun. These unique data are available thanks to the long-term dedicated efforts of the Mount Wilson Observatory HK project, the Lowell Observatory Solar-Stellar Spectrograph, and the National Solar Observatory/Air Force Research Laboratory/Sacremento Peak K-line monitoring program. The Ca II H & K emission originates in the lower chromosphere and is strongly correlated with the presence of magnetic plage regions in the Sun. These synoptic observations allow us to trace the patterns long-term magnetic variability and explore dynamo behavior over a wide range of rotation regimes and stellar evolution timescales.

  12. Témoignage : « Mon père était avec Leclerc »

    OpenAIRE

    Doughty, Robert

    2008-01-01

    Le 250e bataillon d’artillerie de l’armée américaine a été entraîné à Paris, au Texas, et a débarqué à la fin juillet 1944 sur la plage de Utah. Au début août, le bataillon devait constituer le support d’artillerie de la 2e division blindée française dans la bataille de Falaise puis couvrir son avancée en direction du Mans et de Strasbourg. Le bataillon fut récompensé par les Français : les soldats reçurent 20 Croix de guerre et furent autorisés à porter la fourragère aux couleurs de la Croix...

  13. Observing Episodic Coronal Heating Events Rooted in Chromospheric Activity

    CERN Document Server

    McIntosh, Scott W

    2009-01-01

    We present results of a multi-wavelength study of episodic plasma injection into the corona of AR 10942. We exploit long-exposure images of the Hinode and Transition Region and Coronal Explorer (TRACE) spacecraft to study the properties of faint, episodic, "blobs" of plasma that are propelled upward along coronal loops that are rooted in the AR plage. We find that the source location and characteristic velocities of these episodic upflow events match those expected from recent spectroscopic observations of faint coronal upflows that are associated with upper chromospheric activity, in the form of highly dynamic spicules. The analysis presented ties together observations from coronal and chromospheric spectrographs and imagers, providing more evidence of the connection of discrete coronal mass heating and injection events with their source, dynamic spicules, in the chromosphere.

  14. Molecular absorption in transition region spectral lines

    CERN Document Server

    Schmit, Donald; Ayres, Thomas; Peter, Hardi; Curdt, Werner; Jaeggli, Sarah

    2014-01-01

    Aims: We present observations from the Interface Region Imaging Spectrograph (IRIS) of absorption features from a multitude of cool atomic and molecular lines within the profiles of Si IV transition region lines. Many of these spectral lines have not previously been detected in solar spectra. Methods: We examined spectra taken from deep exposures of plage on 12 October 2013. We observed unique absorption spectra over a magnetic element which is bright in transition region line emission and the ultraviolet continuum. We compared the absorption spectra with emission spectra that is likely related to fluorescence. Results: The absorption features require a population of sub-5000 K plasma to exist above the transition region. This peculiar stratification is an extreme deviation from the canonical structure of the chromosphere-corona boundary . The cool material is not associated with a filament or discernible coronal rain. This suggests that molecules may form in the upper solar atmosphere on small spatial scales...

  15. 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...

  16. Le référent zoulou omniprésent

    Directory of Open Access Journals (Sweden)

    Frédéric Giraut

    2010-09-01

    Full Text Available Illustration 1 – Ephémère mémorial à la gloire de Shaka sur la plage de DurbanAuteur :  Said Boujrouf, Durban, octobre 2007.En tant qu'épopée d'un royaume précolonial conquérant et éphémère vainqueur de l'armée coloniale britannique, l'histoire zouloue avec son mythique chef Shaka a été érigée en mythe par les colonisés d’Afrique australe et par les colons britanniques et afrikaners. L'histoire guerrière a été mise scène de différents points de vue et à travers différents médias (cinéma, télé...

  17. High resolution telescope and spectrograph observations of solar fine structure in the 1600 A region

    Science.gov (United States)

    Cook, J. W.; Brueckner, G. E.; Bartoe, J.-D. F.

    1983-01-01

    High spatial resolution spectroheliograms of the 1600 A region obtained during the HRTS rocket flight of 1978 February 13 are presented. The morphology, fine structure, and temporal behavior of emission bright points (BPs) in active and quiet regions are illustrated. In quiet regions, network elements persist as morphological units, although individual BPs may vary in intensity while usually lasting the flight duration. In cell centers, the BPs are highly variable on a 1 minute time scale. BPs in plages remain more constant in brightness over the observing sequence. BPs cover less than 4 percent of the quiet surface. The lifetime and degree of packing of BPs vary with the local strength of the magnetic field.

  18. Usinage des Composites par Jet d'eau Abrasif

    OpenAIRE

    Cénac, François; Collombet, Francis; Zitoune, Rédouane; Déléris, Michel

    2011-01-01

    International audience; Le protocole expérimental de fraisage par jet d'eau abrasif obtenu sur aluminium est adapté aux matériaux composites. On met en exergue deux différences majeures liées à l'effet du JEA entre les composites et l'aluminium que sont l'usinabilité et les variabilités. L'usinabilité des matériaux composites étant plus grande que celle de l'aluminium pour le JEA, on propose des plages de paramètres différentes pour les composites, du fait des limitations des machines standar...

  19. La préhistoire en Vendée de la pierre au bronze

    OpenAIRE

    Le Roux, Charles-Tanguy

    2012-01-01

    La Vendée est un département à l’identité forte mais multiforme, très proche de la Bretagne et de la basse vallée de la Loire au nord mais évoquant déjà le Bassin Aquitain dans sa partie méridionale tandis que, d’est en ouest, on passe des collines des Mauges à une alternance de grandes plages, de falaises basses et de zones marécageuses. Ce faible relief du littoral comme des fonds marins qui le précèdent va de pair avec une grande instabilité du trait de côte en fonction de l’érosion-sédime...

  20. 70 years of Sunspot Observations at Kanzelh\\"ohe Observatory: systematic study of parameters affecting the derivation of the relative sunspot number

    CERN Document Server

    Pötzi, Werner; Temmer, Manuela; Baumgartner, Dietmar; Freislich, Heinrich; Strutzmann, Heinz

    2015-01-01

    Kanzelh\\"ohe Observatory (KSO) was founded during World War II by the "Deutsche Luftwaffe" (German Airforces) as one station of a network of observatories, which should provide information on solar activity in order to better assess the actual conditions of the Earth's ionosphere in terms of radio wave propagation. The solar observations began in 1943 with photographs of the photosphere, drawings of sunspots, plage regions and faculae, as well as patrol observations of the solar corona. At the beginning all data was sent to Freiburg (Germany). After WWII international cooperation was established and the data was sent to Zurich, Paris, Moscow and Greenwich. Relative sunspot numbers are derived since 1944. The agreement between relative sunspot numbers derived at KSO and the new International Sunspot Number (ISN) \\citep{SIDC} lies within $\\sim10\\%$. However, revisiting the historical data, we also find periods with larger deviations. The reasons for the deviations were twofold: (1) On the one hand a major instr...

  1. Radial velocity signatures of Zeeman broadening

    CERN Document Server

    Reiners, Ansgar; Anglada-Escude, Guillem; Jeffers, Sandra V; Morin, Julien; Zechmeister, Mathias; Kochukhov, Oleg; Piskunov, Nikolai

    2013-01-01

    Stellar activity signatures such as spots and plage can significantly limit the search for extrasolar planets. Current models of activity-induced radial velocity (RV) signals focused on the impact of temperature contrast in spots predicting the signal to diminish toward longer wavelengths. On the other hand, the relative importance of the Zeeman effect on RV measurements should grow with wavelength, because the Zeeman displacement itself grows with \\lambda, and because a magnetic and cool spot contributes more to the total flux at longer wavelengths. We model the impact of active regions on stellar RV measurements including both temperature contrast in spots and Zeeman line broadening. We calculate stellar line profiles using polarized radiative transfer models including atomic and molecular Zeeman splitting from 0.5 to 2.3\\mum. Our results show that the amplitude of the RV signal caused by the Zeeman effect alone can be comparable to that caused by temperature contrast. Furthermore, the RV signal caused by c...

  2. Multiple Scattering of Seismic Waves from Ensembles of Upwardly Lossy Thin Flux Tubes

    CERN Document Server

    Hanson, Chris S

    2015-01-01

    Our previous semi-analytic treatment of f- and p-mode multiple scattering from ensembles of thin flux tubes (Hanson and Cally, Astrophys. J. 781, 125; 791, 129, 2014) is extended by allowing both sausage and kink waves to freely escape at the top of the model using a radiative boundary condition there. As expected, this additional avenue of escape, supplementing downward loss into the deep solar interior, results in substantially greater absorption of incident f- and p-modes. However, less intuitively, it also yields mildly to substantially smaller phase shifts in waves emerging from the ensemble. This may have implications for the interpretation of seismic data for solar plage regions, and in particular their small measured phase shifts.

  3. A Wave Scattering Theory of Solar Seismic Power Haloes

    CERN Document Server

    Hanasoge, Shravan M

    2009-01-01

    Spatial maps of the high-pass frequency filtered time-averaged root-mean-squared (RMS) Doppler velocities tend to show substantial decrements within regions of strong field and curiously, randomly distributed patches of enhancement in the vicinity. We propose that these haloes or enhancements are a consequence of magnetic-field-induced mode mixing (scattering), resulting in the preferential powering of waves that possess strong surface velocity signatures (i.e. scattering from low to high wavenumbers). Evidently, this process can occur in the reverse, and therefore in order to determine if the haloes are indeed caused by mode mixing, we must answer the question: {\\it how are acoustic waves scattered by magnetic fields?} Through simulations of the interactions between waves and sunspots and models of plage, we demonstrate that the high to low modal order scattering channels are favoured. With increasing frequency and consequently, decreasing wavelength, a growing number of modes are scattered by the sunspot, t...

  4. 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.

  5. Axisymmetric absorption of p modes by an ensemble of thin, magnetic-flux tubes

    Energy Technology Data Exchange (ETDEWEB)

    Jain, R; Gascoyne, A [Department of Applied Mathematics, University of Sheffield (United Kingdom); Hindman, B W, E-mail: R.Jain@sheffield.ac.uk [JILA, University of Colorado at Boulder (United States)

    2011-01-01

    The buffeting action of the solar acoustic waves (p modes) on magnetic fibrils excites magnetohydrodynamic (MHD) tube waves. We model these fibrils as axisymmetric, untwisted, vertically oriented, thin, magnetic-flux tubes. The MHD tube waves propagate along the length of the tube and carry energy away from the p-mode cavity creating a source of p-mode absorption. We calculate the absorption arising from the excitation of sausage MHD waves within a model plage composed of many flux tubes with differing plasma properties. We find that for a collection of tubes with normally distributed plasma parameters {beta}, the macroscopic absorption coefficient of the collection effectively depends on only the mean value of {beta}.

  6. Dimming of the Mid-20th Century Sun

    CERN Document Server

    Foukal, Peter

    2015-01-01

    Advances in understanding of the white light faculae measured at the Royal Greenwich Observatory from 1874 to 1976 suggest that they offer a more direct measure of solar brightening by small diameter photospheric magnetic flux tubes than do chromospheric proxies. Proxies such as the area of Ca K plages, the Mg index or the microwave flux include many dark photospheric structures as well as pores and sunspots. Our reconstruction of variation in total solar irradiance,TSI,based on the faculae indicates that the sun dimmed by almost 0.1 percent in the mid- twentieth century rather than brightening as represented in previous reconstructions. This dimmimg at the sun's highest activity level since the seventeenth century is consistent with the photometric behavior observed in somewhat younger sun like stars. The prolonged TSI decrease may have contributed more to the cooling of climate between about 1940 and 1970 than present models indicate.

  7. Three-dimensional simulations of near-surface convection in main-sequence stars. IV. Effect of small-scale magnetic flux concentrations on centre-to-limb variation and spectral lines

    CERN Document Server

    Beeck, Benjamin; Cameron, Robert H; Reiners, Ansgar

    2015-01-01

    Magnetic fields affect the local structure of the photosphere of stars. They can considerably influence the radiative properties near the optical surface, flow velocities, and the temperature and pressure profiles. We aim at understanding qualitatively the influence of small magnetic flux concentrations in unipolar plage regions on the centre-to-limb variation of the intensity and its contrast and on the shape of spectral line profiles in cool main-sequence stars. We analyse the bolometric and continuum intensity and its angular dependence of 24 radiative magnetohydrodynamic simulations of the near-surface layers of main-sequence stars with six different sets of stellar parameters (spectral types F to early M) and four different average magnetic field strengths (including the non-magnetic case). We also calculated disc-integrated profiles of three spectral lines. The small magnetic flux concentrations formed in the magnetic runs of simulations have a considerable impact on the intensity and its centre-to-limb...

  8. Un modèle numérique de terrain issu d'un logiciel de télédétection

    Directory of Open Access Journals (Sweden)

    Frank VIDAL

    1991-06-01

    Full Text Available Il est possible de créer un modèle numérique de terrain en utilisant les fonctions graphiques d’un logiciel de traitement d’images de télédétection. Un plan d’image est créé par numérisation des principales courbes de niveaux et affectation de couleurs croissantes selon les plages d’altitudes choisies. Après transfert sur 256 niveaux de gris, les altitudes intermédiaires sont calculées par un filtrage moyen sur l’image. Après étalement de dynamique, cette image peut être considérée comme un modèle numérique de terrain, et utilisée dans les fonctions 3D du logiciel.

  9. MHD simulations reveal crucial differences between solar and very-cool star magnetic structures

    CERN Document Server

    Beeck, Benjamin; Reiners, Ansgar

    2011-01-01

    We carried out 3D radiative magnetohydrodynamic simulations of the convective and magnetic structure in the surface layers (uppermost part of the convection zone and photosphere) of main-sequence stars of spectral types F3 to M2. The simulation results were analyzed in terms of sizes and properties of the convection cells (granules) and magnetic flux concentrations as well as velocity, pressure, density, and temperature profiles. Our numerical simulations show for the first time a qualitative difference in the magneto-convection between solar-like stars and M dwarfs. Owing to higher surface gravity, lower opacity (resulting in higher density at optical depth unity), and more stable downflows, small-scale magnetic structures concentrate into pore-like configurations of reduced intensity. This implies that in very cool stars magnetic surface structures like plage regions and starspots significantly differ from the solar example. Such a difference would have major impact on the interpretation of Doppler imaging ...

  10. H-alpha features with hot onsets. II. A contrail fibril

    CERN Document Server

    Rutten, R J

    2016-01-01

    The solar chromosphere observed in H-alpha consists mostly of narrow fibrils. The longest typically originate in network or plage and arch far over adjacent internetwork. We use data from multiple telescopes to analyze one well-observed example in a quiet area. It resulted from the earlier passage of an accelerating disturbance in which the gas was heated to high temperature as in the spicule-II phenomenon. After this passage a dark H-Halpha fibril appeared as a contrail. We use Saha-Boltzmann extinction estimation to gauge the onset and subsequent visibilities in various diagnostics and conclude that such H-alpha fibrils can indeed be contrail phenomena, not indicative of the thermodynamic and magnetic environment when they are observed but of more dynamic happenings before. They do not connect across internetwork cells but represent launch tracks of heating events and chart magnetic field during launch, not at present.

  11. Sequential Chomospheric Brightening: An Automated Approach to Extracting Physics from Ephemeral Brightening

    CERN Document Server

    Kirk, Michael S; Jackiewicz, Jason; McAteer, R T James; McNamara, Bernie J

    2012-01-01

    We make a comparison between small scale chromospheric brightenings and energy release processes through examining the temporal evolution of sequential chromospheric brightenings (SCBs), derive propagation velocities, and propose a connection of the small-scale features to solar flares. Our automated routine detects and distinguishes three separate types of brightening regularly observed in the chromosphere: plage, flare ribbon, and point brightenings. By studying their distinct dynamics, we separate out the flare-associated bright points commonly known as SCBs and identify a propagating Moreton wave. Superimposing our detections on complementary off-band images, we extract a Doppler velocity measurement beneath the point brightening locations. Using these dynamic measurements, we put forward a connection between point brightenings, the erupting flare, and overarching magnetic loops. A destabilization of the pre-flare loop topology by the erupting flare directly leads to the SCBs observed.

  12. Magnetohydrodynamic waves driven by p-modes

    CERN Document Server

    Khomenko, Elena

    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. 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.

  14. Temporal Variation of Ca–K Line Profile of the Sun during the Solar Cycle 22 and 23

    Indian Academy of Sciences (India)

    G. Sindhuja; Jagdev Singh

    2015-03-01

    We obtained the Ca–K line profile of the Sun as a star since 1969 at the Kodaikanal Observatory (KO) and analysis of the data showed the need to delineate the role of different chromospheric features to the variations of solar irradiance. We, therefore, initiated a new methodology to make observations of Ca–K line profiles of the Sun as a function of latitude and integrated over the longitude on a daily basis since 1986. We have collected the data for about thousand days, spread over two solar cycles. Earlier data (before 1997) were recorded on the photographic film and later data using the CCD detector. The photographic film data were digitized and analysed along with the data obtained from CCD camera. From these data, we computed K1 and K2 widths for the Sun as a star, using all the observed line profiles as a function of latitude. In addition, we have analyzed the spectra of the whole Sun as a star obtained on some days and compared it with the results obtained from latitude spectra of the same day. The K1 and K2 widths of the Sun as a star derived from the KO data are compared with values determined from the observations made at other observatories to compare results from the new methodology of observations adopted by us and the earlier techniques. The average values of K1 width during the minimum period. of solar cycle 23 are smaller than those during the minimum period of cycle 22. Day-to-day variations in the K1 and K2 widths and plage areas may imply that irradiance variations occur not only due to large-scale solar activity, but also because of variations in some of the three types of network in quiet regions of the Sun. The variation in intensity of the plages can also cause day-to-day variations in widths.

  15. Suppression of Heating of Coronal Loops Rooted in Opposite Polarity Sunspot Umbrae

    Science.gov (United States)

    Tiwari, Sanjiv K.; Thalmann, Julia K.; Moore, Ronald L.; Panesar, Navdeep K.; Winebarger, Amy R.

    2016-01-01

    EUV observations of active region (AR) coronae reveal the presence of loops at different temperatures. To understand the mechanisms that result in hotter or cooler loops, we study a typical bipolar AR, near solar disk center, which has moderate overall magnetic twist and at least one fully developed sunspot of each polarity. From AIA 193 and 94 Å images we identify many clearly discernible coronal loops that connect plage or a sunspot of one polarity to an opposite-­polarity plage region. The AIA 94 Å images show dim regions in the umbrae of the spots. To see which coronal loops are rooted in a dim umbral area, we performed a non-linear force-free field (NLFFF) modeling using photospheric vector magnetic field measurements obtained with the Heliosesmic Magnetic Imager (HMI) onboard SDO. The NLFFF model, validated by comparison of calculated model field lines with observed loops in AIA 193 and 94 Å, specifies the photospheric roots of the model field lines. Some model coronal magnetic field lines arch from the dim umbral area of the positive-polarity sunspot to the dim umbral area of a negative-polarity sunspot. Because these coronal loops are not visible in any of the coronal EUV and X-ray images of the AR, we conclude they are the coolest loops in the AR. This result suggests that the loops connecting opposite polarity umbrae are the least heated because the field in umbrae is so strong that the convective braiding of the field is strongly suppressed.

  16. Chromospheric activity on the late-type star V1355 Ori using Lijiang 1.8-m and 2.4-m telescopes

    Science.gov (United States)

    Pi, Qing-Feng; Zhang, Li-Yun; Chang, Liang; Han, Xian-Ming; Lu, Hong-Peng; Zhang, Xi-Liang; Wang, Dai-Mei

    2016-10-01

    We obtained new high-resolution spectra using the Lijiang 1.8-m and 2.4-m telescopes to investigate the chromospheric activities of V1355 Ori as indicated in the behaviors of Ca ii H&K, Hδ, Hγ, Hβ, Na i D1, D2, Hα and Ca ii infrared triplet (IRT) lines. The observed spectra show obvious emissions above the continuum in Ca ii H&K lines, absorptions in the Hδ, Hγ, Hβ and Na i D1, D2 lines, variable behavior (filled-in absorption, partial emission with a core absorption component or emission above the continuum) in the Hα line, and weak self-reversal emissions in the strong filled-in absorptions of the Ca ii IRT lines. We used a spectral subtraction technique to analyze our data. The results show no excess emission in the Hδ and Hγ lines, very weak excess emissions in the Na i D1, D2 lines, excess emission in the Hβ line, clear excess emission in the Hα line, and excess emissions in the Ca ii IRT lines. The value of the ratio of EW8542/EW8498 is in the range 0.9 to 1.7, which implies that chromospheric activity might have been caused by plage events. The value of the ratio E Hα/E Hβ is above 3, indicating that the Balmer lines would arise from prominence-like material. We also found time variations in light curves associated with equivalent widths of chromospheric activity lines in the Na i D1, D2, Ca ii IRT and Hα lines in particular. These phenomena can be explained by plage events, which are consistent with the behavior of chromospheric activity indicators.

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

    Energy Technology Data Exchange (ETDEWEB)

    Jain, Rekha; Gascoyne, Andrew [School of Mathematics and Statistics, University of Sheffield, Sheffield S3 7RH (United Kingdom); Hindman, Bradley W.; Greer, Benjamin, E-mail: R.Jain@sheffield.ac.uk [JILA, University of Colorado, Boulder, CO 80309-0440 (United States)

    2014-12-01

    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.

  18. 1993年5月日面AR7500中暗条的动力学特征%The Dynamical Feature of Filaments in AR7500

    Institute of Scientific and Technical Information of China (English)

    姜云春; 栾蒂

    2001-01-01

    An analysis of the evolution and dynamical feature of three filaments using the magnetogram of photosphere and Hβ Dopplergrams of chromosphere in AR7500 on May,1993 is presented in this paper.Conclusions are as follows:1)There are two dextral and a sinistral in three filaments.They constitude two cusps.One of the cusp is rooted in positive polarity plage region,which has blueshift motion and velocity cusp.While the other in a small decaying spot with negitive polority has redshift motion.The both ends in other side extend into the big negative polarity sunspot and positive polarity plage region respectively.The red and blue-shift motions of these cusps and both ends exist 24 hours continually.2)Both chromospheric plage associated fibrils near the filament and the transverse magnetic field of the photosphere beneath the filaments almost parallel to the long axis of these filaments.The sunspot of the end does not present obvious spiral structure.The orientations of the field along with the axis are different in these three filaments,and the possible direction of the flow of the electric current is identical.There are matter motion along the direction of the axis of magnetic field in two filaments,but this has no relationship with the difference of the handedness;it has symmetrical fall motion in the axis direction at the other dextral filaments of trouble activation.3)The axis field has different direction in cusp so that it does not always occur with merge of filament,as a dextral filament disappears and forms again.When two sinistral and dextral filaments disintegrate into parallel fibrils which connect the same positive or negative polarity,their cusps clearly exist due to the different handedness.4).The sinistral filament exists during several days,but no trouble activation in the two observing days.A dextral filament has trouble activation and “relaxing” turning round before disappearance.The other dextral filament exists for a long term presenting obvious

  19. Watching the Sun to Improve Exoplanet Detection

    Science.gov (United States)

    Kohler, Susanna

    2015-12-01

    Looking for stars that wobble is one of the key ways by which we detect exoplanets: the gravitational pull of planets cause tiny variations in stars radial velocities. But our ability to detect Earth twins is currently limited by our ability to distinguish between radial-velocity variations caused by exoplanets, and those caused by noise from the star itself. A team of scientists has recently proposed that the key to solving this problem may be to examine our own star.Precision Amid NoiseThe radial-velocity technique works well for detecting large planets on close orbits, but detecting an Earth twin requires being able to detect star motion on the order of 10 cm/s! This precision is hard to reach, because activity on the stellar surface i.e., sunspots, plages (bright spots), or granulation can also cause variations in the measured radial velocity for the star, obscuring the signature of a planet.Because the stars were examining arent resolved, we cant track the activity on their surfaces so how can we better understand the imprint that stellar activity has on radial-velocity measurements? A team of scientists has come up with a clever approach: examine the Sun as though it were a distant star.Wealth of InformationThe team, led by Xavier Dumusque (Branco-Weiss Fellow at the Harvard-Smithsonian Center for Astrophysics) and David F. Phillips (Harvard-Smithsonian Center for Astrophysics), has begun a project to observe the Sun with a ground-based solar telescope. The telescope observes the full disk of the Sun and feeds the data into the HARPS-N spectrograph in Spain, a spectrograph normally used for radial-velocity measurements of other stars in the hunt for exoplanets.But the team has access to other data about the Sun, too: information from satellites like the Solar Dynamics Observatory and SORCE about the solar activity and total irradiance during the time when the spectra were taken. Dumusque and collaborators have combined all of this information, during a week

  20. 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.

  1. 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

  2. Time-dependent Suppression of Oscillatory Power in Evolving Solar Magnetic Fields

    Science.gov (United States)

    Krishna Prasad, S.; Jess, D. B.; Jain, R.; Keys, P. H.

    2016-05-01

    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 Hα 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.

  3. WHAT CAUSES THE INTER-SOLAR-CYCLE VARIATION OF TOTAL SOLAR IRRADIANCE?

    Energy Technology Data Exchange (ETDEWEB)

    Xiang, N. B.; Kong, D. F., E-mail: nanbin@ynao.ac.cn [National Astronomical Observatories/Yunnan Observatory, CAS, Kunming 650011 (China)

    2015-12-15

    The Physikalisch Meteorologisches Observatorium Davos total solar irradiance (TSI), Active Cavity Radiometer Irradiance Monitoring TSI, and Royal Meteorological Institute of Belgium TSI are three typical TSI composites. Magnetic Plage Strength Index (MPSI) and Mount Wilson Sunspot Index (MWSI) should indicate the weak and strong magnetic field activity on the solar full disk, respectively. Cross-correlation (CC) analysis of MWSI with three TSI composites shows that TSI should be weakly correlated with MWSI, and not be in phase with MWSI at timescales of solar cycles. The wavelet coherence (WTC) and partial wavelet coherence (PWC) of TSI with MWSI indicate that the inter-solar-cycle variation of TSI is also not related to solar strong magnetic field activity, which is represented by MWSI. However, CC analysis of MPSI with three TSI composites indicates that TSI should be moderately correlated and accurately in phase with MPSI at timescales of solar cycles, and that the statistical significance test indicates that the correlation coefficient of three TSI composites with MPSI is statistically significantly higher than that of three TSI composites with MWSI. Furthermore, the cross wavelet transform (XWT) and WTC of TSI with MPSI show that the TSI is highly related and actually in phase with MPSI at a timescale of a solar cycle as well. Consequently, the CC analysis, XWT, and WTC indicate that the solar weak magnetic activity on the full disk, which is represented by MPSI, dominates the inter-solar-cycle variation of TSI.

  4. 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

  5. Density diagnostics derived from the OIV and SIV intercombination lines observed by IRIS

    CERN Document Server

    Polito, V; Dudík, J; Mason, H E; Giunta, A; Reeves, K K

    2016-01-01

    The intensity of the \\oiv~2s$^{2}$ 2p $^{2}$P-2s2p$^{2}$ $^{4}$P and \\siv~3 s$^{2}$ 3p $^{2}$P- 3s 3p$^{2}$ $^{4}$ P intercombination lines around 1400~\\AA~observed with the \\textit{Interface Region Imaging Spectrograph} (IRIS) provide a useful tool to diagnose the electron number density ($N_\\textrm{e}$) in the solar transition region plasma. We measure the electron number density in a variety of solar features observed by IRIS, including an active region (AR) loop, plage and brightening, and the ribbon of the 22-June-2015 M 6.5 class flare. By using the emissivity ratios of \\oiv\\ and \\siv\\ lines, we find that our observations are consistent with the emitting plasma being near isothermal (log$T$[K] $\\approx$ 5) and iso-density ($N_\\textrm{e}$ $\\approx$~10$^{10.6}$ cm$^{-3}$) in the AR loop. Moreover, high electron number densities ($N_\\textrm{e}$ $\\approx$~10$^{13}$ cm$^{-3}$) are obtained during the impulsive phase of the flare by using the \\siv\\ line ratio. We note that the \\siv\\ lines provide a higher ran...

  6. The Mount Wilson Observatory S-index of the Sun

    CERN Document Server

    Egeland, Ricky; Baliunas, Sallie; Hall, Jeffrey C; Pevtsov, Alexei A; Bertello, Luca

    2016-01-01

    The most commonly used index of stellar magnetic activity is the instrumental flux scale of singly-ionized calcium H & K line core emission, S, developed by the Mount Wilson Observatory (MWO) HK Project, or the derivative index R'_HK. Accurately placing the Sun on the S scale is important for comparing solar activity to that of the Sun-like stars. We present previously unpublished measurements of the reflected sunlight from the Moon using the second-generation MWO HK photometer during solar cycle 23 and determine cycle minimum S_min,23 = 0.1634 +/- 0.0008, amplitude Delta S_23 = 0.0143 +/- 0.0015, and mean = 0.1701 +/- 0.0005. By establishing a proxy relationship with the closely related National Solar Observatory Sacramento Peak calcium K emission index, itself well-correlated with the Kodaikanal Observatory plage index, we extend the MWO S time series to cover cycles 15-24 and find on average = 0.1621 +/- 0.0008, = 0.0145 +/- 0.0012, = 0.1694 +/- 0.0005. Our measurements represent an improvement ove...

  7. Chromospheric activity and rotational modulation of the RS Canum Venaticorum binary V711 Tauri during 1998-2004

    Science.gov (United States)

    Cao, Dongtao; Gu, Shenghong

    2015-05-01

    We present long-term high-resolution spectroscopic observations of the very active RS Canum Venaticorum-type star V711 Tau, obtained during several observing runs from 1998 to 2004, and study its chromospheric activity. Using the spectral subtraction technique, several optical chromospheric activity indicators [including the He I D3, Na I D1, D2, Hα and Ca II infrared triplet (IRT) lines] formed at different atmospheric heights are analysed. Strong chromospheric emission supports earlier results that indicate that V711 Tau is a very active system. Two large optical flares were detected during our observations. The results suggest that the main part of chromospheric emission is attributed to the primary star of the system. The secondary also presents weak emission but is less active. The ratios of EW8542/EW8498 indicate that Ca II IRT emission arises predominantly from plage-like regions. We have found rotational modulation of chromospheric activity in the Hα and Ca II IRT lines, which suggests the presence of the chromospheric active longitudes over the surface of V711 Tau. Two active longitudes separated by about 180° were observed to dominate the activity, and the so-called flip-flop phenomenon was seen during our observations. Moreover, the chromospheric activity level shows a long-term variation that gradually increases from a deep minimum near the year 2002. A close spatial connection of photospheric spots and chromospheric active regions in both short and long timescales was found for V711 Tau.

  8. 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.

  9. 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’&...

  10. Is it possible to detect planets around young active G and K dwarfs?

    CERN Document Server

    Jeffers, S V; Jones, H R A; Reiners, A; Pinfield, D J; Marsden, S C

    2013-01-01

    Theoretical predictions suggest that the distribution of planets in very young stars could be very different to that typically observed in Gyr old systems that are the current focus of radial velocity surveys. However, the detection of planets around young stars is hampered by the increased stellar activity associated with young stars, the signatures of which can bias the detection of planets. In this paper we place realistic limitations on the possibilities for detecting planets around young active G and K dwarfs. The models of stellar activity based on tomographic imaging of the G dwarf HD 141943 and the K1 dwarf AB Dor and also include contributions from plage and many small random starspots. Our results show that the increased stellar activity levels present on young Solar-type stars strongly impacts the detection of Earth-mass and Jupiter mass planets and that the degree of activity jitter is directly correlated with stellar \\vsinis. We also show that for G and K dwarfs, the distribution of activity in i...

  11. A comparison of gene set analysis methods in terms of sensitivity, prioritization and specificity.

    Directory of Open Access Journals (Sweden)

    Adi L Tarca

    Full Text Available Identification of functional sets of genes associated with conditions of interest from omics data was first reported in 1999, and since, a plethora of enrichment methods were published for systematic analysis of gene sets collections including Gene Ontology and biological pathways. Despite their widespread usage in reducing the complexity of omics experiment results, their performance is poorly understood. Leveraging the existence of disease specific gene sets in KEGG and Metacore® databases, we compared the performance of sixteen methods under relaxed assumptions while using 42 real datasets (over 1,400 samples. Most of the methods ranked high the gene sets designed for specific diseases whenever samples from affected individuals were compared against controls via microarrays. The top methods for gene set prioritization were different from the top ones in terms of sensitivity, and four of the sixteen methods had large false positives rates assessed by permuting the phenotype of the samples. The best overall methods among those that generated reasonably low false positive rates, when permuting phenotypes, were PLAGE, GLOBALTEST, and PADOG. The best method in the category that generated higher than expected false positives was MRGSE.

  12. Observed Variability of the Solar Mg II h Spectral Line

    CERN Document Server

    Schmit, Donald; De Pontieu, Bart; McIntosh, Scott; Leenaarts, Jorrit; Carlsson, Mats

    2015-01-01

    The Mg II h&k doublet are two of the primary spectral lines observed by the Sun-pointing Interface Region Imaging Spectrograph (IRIS). These lines are tracers of the magnetic and thermal environment that spans from the photosphere to the upper chromosphere. We use a double gaussian model to fit the Mg II h profile for a full-Sun mosaic dataset taken 24-Aug-2014. We use the ensemble of high-quality profile fits to conduct a statistical study on the variability of the line profile as it relates the magnetic structure, dynamics, and center-to-limb viewing angle. The average internetwork profile contains a deeply reversed core and is weakly asymmetric at h2. In the internetwork, we find a strong correlation between h3 wavelength and profile asymmetry as well h1 width and h2 width. The average reversal depth of the h3 core is inversely related to the magnetic field. Plage and sunspots exhibit many profiles which do not contain a reversal. These profiles also occur infrequently in the internetwork. We see indic...

  13. The Solar Dynamo Zoo

    Science.gov (United States)

    Egeland, Ricky; Soon, Willie; Baliunas, Sallie; Hall, Jeffrey C.; Pevtsov, Alexei A.; Henry, Gregory W.

    2016-07-01

    We present composite time series of Ca II H & K line core emission indices of up to 50 years in length for a set of 27 solar-analog stars (spectral types G0-G5; within 10% of the solar mass) and the Sun. These unique data are available thanks to the long-term dedicated efforts of the Mount Wilson Observatory HK project, the Lowell Observatory Solar-Stellar Spectrograph, and the National Solar Observatory/Air Force Research Laboratory/Sacramento Peak K-line monitoring program. The Ca II H & K emission originates in the lower chromosphere and is strongly correlated with the presence of magnetic plage regions in the Sun. These synoptic observations allow us to trace the patterns long-term magnetic variability and explore dynamo behavior over a wide range of rotation regimes and stellar evolution timescales.In this poster, the Ca HK observations are expressed using the Mount Wilson S-index. Each time series is accompanied by a Lomb-Scargle periodogram, fundemental stellar parameters derived from the Geneva-Copenhagen Survey, and statistics derived from the time series including the median S-index value and seasonal and long-term amplitudes. Statistically significant periodogram peaks are ranked according to a new cycle quality metric. We find that clear, simple, Sun-like cycles are the minority in this sample.

  14. Construction of a Ca II Core-to-Wing Ratio Image

    Science.gov (United States)

    Roberts, H.

    2015-12-01

    To understand Earth's climate, we must first understand the Sun. However, there are still significant uncertainties associated with both the fundamental mechanisms of solar variability and how they enter into the Earth's climate system. An important method to study the causes of solar variability can be found through the analysis of solar images. The Precision Solar Photometric Telescope (PSPT) located at the Mauna Loa Solar Observatory (MLSO) acquires images of the Sun in three different photometric bands to monitor the evolution of solar surface features that change over the course of a solar cycle. These images provide a complete knowledge about the Sun by targeting different layers of the solar atmosphere. Though raw images are meaningful and important, precision image processing is required to remove instrumental artifacts and false features that may appear in these images prior to usage for scientific purposes. A scientific application of the high precision solar images is investigated by analyzing a set of narrow band of Calcium II K core and wing images. The Core and Wing images are processed to remove the influence of the center-to-limb variation; the resultant core-to-wing ratio image enhances the appearance of network structures on the entire solar disk along with the more obvious facula and plage brightening associated with the passage of active regions.

  15. Ubiquitous High Speed Transition Region and Coronal Upflows in the Quiet Sun

    CERN Document Server

    Mcintosh, Scott W

    2009-01-01

    We study the line profiles of a range of transition region (TR) emission lines observed in typical quiet Sun regions. In magnetic network regions, the Si IV 1402\\AA{}, C IV 1548\\AA{}, N V 1238\\AA{}, O VI 1031\\AA{}, and Ne VIII 770\\AA{} spectral lines show significant asymmetry in the blue wing of the emission line profiles. We interpret these high-velocity upflows in the lower and upper TR as the quiet Sun equivalent of the recently discovered upflows in the low corona above plage regions (Hara et al., 2008). The latter have been shown to be directly associated with high-velocity chromospheric spicules that are (partially) heated to coronal temperatures and play a significant role in supplying the active region corona with hot plasma (DePontieu et al., 2009}. We show that a similar process likely dominates the quiet Sun network. We provide a new interpretation of the observed quiet Sun TR emission in terms of the relentless mass transport between the chromosphere and corona - a mixture of emission from dynami...

  16. 70 Years of Sunspot Observations at the Kanzelhöhe Observatory: Systematic Study of Parameters Affecting the Derivation of the Relative Sunspot Number

    Science.gov (United States)

    Pötzi, Werner; Veronig, Astrid M.; Temmer, Manuela; Baumgartner, Dietmar J.; Freislich, Heinrich; Strutzmann, Heinz

    2016-11-01

    The Kanzelhöhe Observatory (KSO) was founded during World War II by the Deutsche Luftwaffe (German Airforce) as one station of a network of observatories that were set up to provide information on solar activity in order to better assess the actual conditions of the Earth's ionosphere in terms of radio-wave propagation. Solar observations began in 1943 with photographs of the photosphere and drawings of sunspots, plage regions, and faculae, as well as patrol observations of the solar corona. At the beginning, all data were sent to Freiburg (Germany). After WW II, international cooperation was established and the data were sent to Zurich, Paris, Moscow, and Greenwich. Relative sunspot numbers have been derived since 1944. The agreement between relative sunspot numbers derived at KSO and the new International Sunspot Number (ISN) (SILSO World Data Center in International Sunspot Number Monthly Bulletin and online catalogue, 1945 - 2015) lies within {≈} 10 %. However, revisiting the historical data, we also find periods with larger deviations. The reasons for the deviations were twofold: On the one hand, a major instrumental change took place during which the instrument was relocated and modified. On the other hand, a period of frequent replacements of personnel caused significant deviations; this clearly shows the importance of experienced observers. In the long term, the instrumental improvements led to better image quality. Additionally, we find a long-term trend towards better seeing conditions that began in 2000.

  17. Stray Light Correction of HMI Data

    Science.gov (United States)

    Norton, Aimee Ann; Duvall, Thomas; Schou, Jesper; Cheung, Mark; Scherrer, Philip H.

    2017-08-01

    The point spread function (PSF) for HMI is an Airy function convolved with a Lorentzian. The parameters are bound by ground-based testing before launch, then post-launch off-limb light curves, lunar eclipse and Venus transit data. The PSF correction is programmed in C and runs within the HMI data processing pipeline environment. A single full-disk intensity image can be processed in less than one second. Deconvolution of the PSF on the Stokes profile data (a linear combination of original filtergrms) is less computationally expensive and is shown to be equivalent to deconvolution applied at the original filtergram level. Results include a decrease in umbral darkness of a few percent (~200 K cooler), a doubling of the granulation contrast in intensity from 3.6 to 7.2%, an increase in plage field strengths by a factor of 1.5, and a partial correction of the convective blueshift in Doppler velocities. Requests for data corrected for stray light are welcome and will be processed by the HMI team.

  18. The Mount Wilson Observatory S-index of the Sun

    Science.gov (United States)

    Egeland, Ricky; Soon, Willie; Baliunas, Sallie; Hall, Jeffrey C.; Pevtsov, Alexei A.; Bertello, Luca

    2017-01-01

    The most commonly used index of stellar magnetic activity is the instrumental flux scale of singly ionized calcium H & K line core emission, S, developed by the Mount Wilson Observatory (MWO) HK Project, or the derivative index {R}{HK}\\prime . Accurately placing the Sun on the S scale is important for comparing solar activity to that of the Sun-like stars. We present previously unpublished measurements of the reflected sunlight from the Moon using the second-generation MWO HK photometer during solar cycle 23 and determine cycle minimum {S}23,\\min =0.1634+/- 0.0008, amplitude {{Δ }}{S}23=0.0143+/- 0.0012, and mean =0.1701+/- 0.0005. By establishing a proxy relationship with the closely related National Solar Observatory Sacramento Peak calcium K emission index, itself well correlated with the Kodaikanal Observatory plage index, we extend the MWO S time series to cover cycles 15–24 and find on average =0.1621+/- 0.0008, =0.0145+/- 0.0012, =0.1694+/- 0.0005. Our measurements represent an improvement over previous estimates that relied on stellar measurements or solar proxies with non-overlapping time series. We find good agreement from these results with measurements by the Solar-Stellar Spectrograph at Lowell Observatory, an independently calibrated instrument, which gives us additional confidence that we have accurately placed the Sun on the S-index flux scale.

  19. Short dynamic fibrils in sunspot chromospheres

    CERN Document Server

    van der Voort, Luc Rouppe

    2013-01-01

    Sunspot chromospheres display vigorous oscillatory signature when observed in chromospheric diagnostics like the strong Ca II lines and H-alpha. New high-resolution sunspot observations from the Swedish 1-m Solar Telescope show the ubiquitous presence of small-scale periodic jet-like features that move up and down. This phenomenon has not been described before. Their typical width is about 0.3 arcsec and they display clear parabolic trajectories in space-time diagrams. The maximum extension of the top of the jets is lowest in the umbra, a few 100 km, and progressively longer further away from the umbra in the penumbra, with the longest more than 1000 km. These jets resemble dynamic fibrils found in plage regions but at smaller extensions. LTE inversion of spectro-polarimetric Ca II 8542 observations enabled for a comparison of the magnetic field inclination and the properties of these short jets. We find that the most extended of these jets also have longer periods and tend to be located in regions with more ...

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

    Science.gov (United States)

    Pomares-Estran, Christelle; Delaunay, Pascal; Mottard, Annie; Cua, Eric; Roger, Pierre-Marie; Pradines, Bruno; Parzy, Daniel; Bogreau, Hervé; Rogier, Christophe; Jeannin, Charles; Karch, Saïd; Fontenille, Didier; Dejour-Salamanca, Dominique; Legros, Fabrice; Marty, Pierre

    2009-08-23

    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.

  1. 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.

  2. On the long-term correlation between the flux in the Ca II H & K and Halpha lines for FGK stars

    CERN Document Server

    da Silva, J Gomes; Boisse, I; Dumusque, X; Lovis, C

    2013-01-01

    The re-emission in the cores of the Ca II H & K and H$\\alpha$ lines, are well known proxies of stellar activity. However, these activity indices probe different activity phenomena, the first being more sensitive to plage variation, while the other one being more sensitive to filaments. In this paper we study the long-term correlation between $\\log R'_{HK}$ and $\\log I_{H\\alpha}$, two indices based on the Ca II H & K and H$\\alpha$ lines respectively, for a sample of 271 FGK stars using measurements obtained over a $\\sim$9 year time span. Because stellar activity is one of the main obstacles to the detection of low-mass and long-period planets, understanding further this activity index correlation can give us some hints about the optimal target to focus on, and ways to correct for these activity effects. We found a great variety of long-term correlations between $\\log R'_{HK}$ and $\\log I_{H\\alpha}$. Around 20% of our sample has strong positive correlation between the indices while about 3% show strong ...

  3. Three-dimensional mapping of red stingray ( Dasyatis akajei) movement with reference to bottom topography

    Science.gov (United States)

    Otaki, Takayoshi; Hamana, Masahiro; Tanoe, Hideaki; Miyazaki, Nobuyuki; Shibuno, Takuro; Komatsu, Teruhisa

    2015-06-01

    Most demersal fishes maintain strong relations with bottom substrates and bottom depths and/or topography during their lives. It is important to know these relations to for understand their lives. In Tokyo Bay, red stingray, Dasyatis akajei, classified as near-threatened species by IUCN, has increased since the 1980s. It is a top predator and engages in ecosystem engineer by mixing the sand bed surface through burring behavior, and greatly influences a coastal ecosystem. It is reported that this species invades in plage and tidal flats and has sometimes injured beachgoers and people gathering clams in Tokyo bay. Thus, it is necessary to know its behavior and habitat use to avoid accidents and to better conserve the biodiversity of ecosystems. However, previous studies have not examined its relationship with the bottom environment. This study aims to describe its behavior in relation to the bottom environment. We sounded three dimensional bottom topography of their habitat off Kaneda Cove in Tokyo Bay with interferometric sidescan sonar system and traced the movement of red stingrays by attaching a data logger system to survey their migration. The results revealed that red stingray repeated vertical movement between the surface and bottom, and used not only sand beds but also rocky beds.

  4. Miniature loops in the solar corona

    CERN Document Server

    Barczynski, Krzysztof; Savage, Sabrina L

    2016-01-01

    Magnetic loops filled with hot plasma are the main building blocks of the solar corona. Usually they have lengths of the order of the barometric scale height in the corona that is 50 Mm. Previously it has been suggested that miniature versions of hot loops exist. These would have lengths of only 1 Mm barely protruding from the chromosphere and spanning across just one granule in the photosphere. Such short loops are well established at transition region temperatures (0.1 MK), and we investigate if such miniature loops also exist at coronal temperatures (>1 MK). We used extreme UV imaging (EUV) observations from the High-resolution Coronal Imager (Hi-C) at an unprecedented spatial resolution of 0.3" to 0.4". Together with EUV imaging and magnetogram data from the Solar Dynamics Observatory (SDO) and X-Ray Telescope (XRT) data from Hinode we investigated the spatial, temporal and thermal evolution of small loop-like structures in the solar corona above a plage region close to an active region and compared this ...

  5. Resolving Azimuth Ambiguity Using Vertical Nature of Solar Quiet-Sun Magnetic Fields

    CERN Document Server

    Gosain, Sanjay

    2012-01-01

    The measurement of solar magnetic fields using the Zeeman effect diagnostics has a fundamental 180 degree ambiguity in the determination of the azimuth angle of the transverse field component. There are several methods that are used in the community and each one has its merits and demerits. Here we present a disambiguation idea that is based on the assumption that most of the magnetic field on the sun is predominantly vertical. While the method is not applicable to penumbra or other features harboring predominantly horizontal fields like the sheared neutral lines, it is useful for regions where fields are predominantly vertical like network and plage areas. The method is tested with the full-disk solar vector magnetograms observed by the VSM/SOLIS instrument. We find that statistically about 60-85 % of the pixels in a typical full-disk magnetogram has field inclination in the range of 0-30 degrees with respect to the local solar normal, and thus can be successfully disambiguated by the proposed method. Due to...

  6. Calculations of periodicity from Hα profiles of Proxima Centauri

    Science.gov (United States)

    Collins, John M.; Jones, Hugh R. A.; Barnes, John R.

    2017-06-01

    We investigate retrieval of the stellar rotation signal for Proxima Centauri. We make use of high-resolution spectra taken with UVES and HARPS of Proxima Centauri over a 13-yr period as well as photometric observations of Proxima Centauri from ASAS and HST. We measure the Hα equivalent width and Hα index, skewness and kurtosis and introduce a method that investigates the symmetry of the line, the peak ratio, which appears to return better results than the other measurements. Our investigations return a most significant period of 82.6 ± 0.1 days, confirming earlier photometric results and ruling out a more recent result of 116.6 days which we conclude to be an alias induced by the specific HARPS observation times. We conclude that whilst spectroscopic Hα measurements can be used for period recovery, in the case of Proxima Centauri the available photometric measurements are more reliable. We make 2D models of Proxima Centauri to generate simulated Hα, finding that reasonable distributions of plage and chromospheric features are able to reproduce the equivalent width variations in observed data and recover the rotation period, including after the addition of simulated noise and flares. However the 2D models used fail to generate the observed variety of line shapes measured by the peak ratio. We conclude that only 3D models which incorporate vertical motions in the chromosphere can achieve this.

  7. Preserving a Unique Archive for Long-Term Solar Variability Studies

    Science.gov (United States)

    Webb, David F.; Hewins, Ian; McFadden, Robert; Emery, Barbara; Gibson, Sarah; Denig, William

    2016-05-01

    In 1964 (solar cycle 20) Patrick McIntosh began creating hand-drawn synoptic maps of solar activity, based on Hydrogen alpha (Hα) imaging measurements. These synoptic maps were unique because they traced the polarity inversion lines (PILs), connecting widely separated filaments, fibril patterns and plage corridors to reveal the large-scale organization of the solar magnetic field. He and his assistants later included coronal hole (CH) boundaries to the maps, usually from ground-based He-I 10830 images. They continued making these maps until 2010 (the start of solar cycle 24), yielding more than 40 years (~ 540 Carrington rotations) or nearly four complete solar cycles (SCs) of synoptic maps. The McIntosh collection of maps forms a unique and consistent set of global solar magnetic field data, and are unique tools for studying the structure and evolution of the large-scale solar fields and polarity boundaries, because: 1) they have excellent spatial resolution for defining polarity boundaries, 2) the organization of the fields into long-lived, coherent features is clear, and 3) the data are relatively homogeneous over four solar cycles. After digitization and archiving, these maps -- along with computer codes permitting efficient searches of the map arrays -- will be made publicly available at NOAA’s National Centers for Environmental Information (NCEI) in their final, searchable form. This poster is a progress report of the project so far and some suggested scientific applications.

  8. A Comparison Study of a Solar Active-Region Eruptive Filament and a Neighboring Non-Eruptive Filament

    CERN Document Server

    Jiang, Chaowei; Feng, Xueshang; Hu, Qiang

    2015-01-01

    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 a CESE-MHD-NLFFF code (Jiang & Feng 2013) 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) co-spatial 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 H{\\alpha} 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 ...

  9. Propagation of Alfv\\'enic Waves From Corona to Chromosphere and Consequences for Solar Flares

    CERN Document Server

    Russell, Alexander J B

    2013-01-01

    How do magnetohydrodynamic waves travel from the fully ionized corona, into and through the underlying partially ionized chromosphere, and what are the consequences for solar flares? To address these questions, we have developed a 2-fluid model (of plasma and neutrals) and used it to perform 1D simulations of Alfv\\'en waves in a solar atmosphere with realistic density and temperature structure. Studies of a range of solar features (faculae, plage, penumbra and umbra) show that energy transmission from corona to chromosphere can exceed 20% of incident energy for wave periods of one second or less. Damping of waves in the chromosphere depends strongly on wave frequency: waves with periods 10 seconds or longer pass through the chromosphere with relatively little damping, however, for periods of 1 second or less, a substantial fraction (37%-100%) of wave energy entering the chromosphere is damped by ion-neutral friction in the mid and upper chromosphere, with electron resistivity playing some role in the lower ch...

  10. Fluxtube model atmospheres and Stokes V zero-crossing wavelengths

    CERN Document Server

    Rubio, L R B; Collados, M

    1997-01-01

    First results of the inversion of Stokes I and V profiles from plage regions near disk center are presented. Both low and high spatial resolution spectra of FeI 6301.5 and FeI 6302.5 A obtained with the Advanced Stokes Polarimeter (ASP) have been considered for analysis. The thin flux tube approximation, implemented in an LTE inversion code based on response functions, is used to describe unresolved magnetic elements. The code allows the simultaneous and consistent inference of all atmospheric quantities determining the radiative transfer with the sole assumption of hydrostatic equilibrium. By considering velocity gradients within the tubes we are able to match the full ASP Stokes profiles. The magnetic atmospheres derived from the inversion are characterized by the absence of significant motions in high layers and strong velocity gradients in deeper layers. These are essential to reproduce the asymmetries of the observed profiles. Our scenario predicts a shift of the Stokes V zero-crossing wavelengths which ...

  11. 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.

  12. Canoe-kayak club

    CERN Multimedia

    Club Canoë Kayak

    2011-01-01

    Le Canoë Kayak CERN se mobilise pour les Initiatives Océanes 2011 Depuis 16 ans, l'association Surfrider mène une bataille sans fin contre les déchets qui polluent nos océans, plages, lacs et rivières en organisant, notamment chaque premier weekend du printemps, des opérations de nettoyage et de sensibilisation sur toute l'Europe. En 2010, cela représentait 40’000 participants, 7’500 scolaires, 34 pays et plus de 950 nettoyages. Cette année, le Canoë kayak CERN a souhaité soutenir les Initiatives Océanes en organisant une opération de nettoyage de la jonction (à Genève) jusqu’au Lignon, avec une équipe sur l'eau, en canoë et en kayak et deux équipes longeant les berges. Grâce à 15 de ses membres, cette mobilisation a permis de ramasser près de 5 m3 de d&...

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

    Science.gov (United States)

    De Pontieu, B.; De Moortel, I.; Martinez-Sykora, J.; McIntosh, S. W.

    2017-08-01

    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.

  14. Basal Chromospheric Flux and Maunder Minimum-type Stars: The quiet-Sun Chromosphere as a Universal Phenomenon

    CERN Document Server

    Schroeder, K -P; Martinez, M I Perez; Cuntz, M; Schmitt, J H M M

    2012-01-01

    Aims: We demonstrate the universal character of the quiet-Sun chromosphere among inactive stars (solar-type and giants). By assessing the main physical processes, we shed new light on some common observational phenomena. Methods: We discuss measurements of the solar Mt. Wilson S-index, obtained by the Hamburg Robotic Telescope around the extreme minimum year 2009, and compare the established chromospheric basal Ca II K line flux to the Mt. Wilson S-index data of inactive ("flat activity") stars, including giants. Results: During the unusually deep and extended activity minimum of 2009, the Sun reached S-index values considerably deeper than in any of its previously observed minima. In several brief periods, the Sun coincided exactly with the S-indices of inactive ("flat", presumed Maunder Minimum-type) solar analogues of the Mt. Wilson sample; at the same time, the solar visible surface was also free of any plages or remaining weak activity regions. The corresponding minimum Ca II K flux of the quiet Sun and ...

  15. Active Region Oscillations: Results from SOHO JOP 097

    Science.gov (United States)

    O'Shea, E.; Fleck, B.; Muglach, K.; Sütterlin, P.

    2001-05-01

    We present here an analysis of data obtained in a sunspot region, using the Coronal Diagnostic Spectrometer (CDS) on SOHO. These data were obtained in the context of the Joint Observing Program (JOP) 97 which, together with CDS, included the Michelson Doppler Imaging (MDI) instrument on SOHO, the TRACE satellite and various ground based observatories, e.g. the DOT on La Palma. Using the lines of Fe XVI 335, Mg IX 368, He I 584, O III 599, Mg X 624 and O V 624 of CDS time series data were obtained in the pore and plage regions of sunspots associated with active regions AR 9166, 9166 and 9169 between September 19-29 2000. In addition to the time series datasets we also obtained 240 arcsec x 240 arcsec raster images of the sunspot regions examined. Using different time series analysis techniques we analyse the different periods of oscillation found in time series datasets and present the results here. This research is part of the European Solar Magnetometry Network supported by the EC through the TMR programme.

  16. Excitation of an Outflow From the Lower Solar Atmosphere and a Co-Temporal EUV Transient Brightening

    CERN Document Server

    Nelson, C J

    2013-01-01

    We analyse an absorption event within the H$\\alpha$ line wings, identified as a surge, and the co-spatial evolution of an EUV brightening, with spatial and temporal scales analogous to a small blinker. We conduct a multi-wavelength, multi-instrument analysis using high-cadence, high-resolution data, collected by the Interferometric BIdimensional Spectrometer on the Dunn Solar Telescope, as well as the space-borne Atmospheric Imaging Assembly and Helioseismic and Magnetic Imager instruments onboard the Solar Dynamics Observatory. One large absorption event situated within the plage region trailing the lead sunspot of AR 11579 is identified within the H-alpha line wings. This event is found to be co-spatially linked to a medium-scale (around 4 arcseconds in diameter) brightening within the transition region and corona. This ejection appears to have a parabolic evolution, first forming in the H-alpha blue wing before fading and reappearing in the H-alpha red wing, and comprises of a number of smaller fibril even...

  17. Surface-focused Seismic Holography of Sunspots: I. Observations

    CERN Document Server

    Braun, D C

    2008-01-01

    We present a comprehensive set of observations of the interaction of p-mode oscillations with sunspots using surface-focused seismic holography. Maps of travel-time shifts, relative to quiet-Sun travel times, are shown for incoming and outgoing p modes as well as their mean and difference. We compare results using phase-speed filters with results obtained with filters that isolate single p-mode ridges, and further divide the data into multiple temporal frequency bandpasses. The f mode is removed from the data. The variations of the resulting travel-time shifts with magnetic-field strength and with the filter parameters are explored. We find that spatial averages of these shifts within sunspot umbrae, penumbrae, and surrounding plage often show strong frequency variations at fixed phase speed. In addition, we find that positive values of the mean and difference travel-time shifts appear exclusively in waves observed with phase-speed filters that are dominated by power in the low-frequency wing of the p1 ridge....

  18. f-mode interaction with models of sunspot: near-field scattering and multifrequency effects

    Science.gov (United States)

    Daiffallah, Khalil

    2016-07-01

    We use numerical simulations to investigate the interaction of an f-mode wave packet with small and large models of a sunspot in a stratified atmosphere. While a loose cluster model has been largely studied before, we focus in this study on the scattering from an ensemble of tightly compact tubes. We showed that the small compact cluster produces a slight distorted scattered wave field in the transverse direction, which can be attributed to the simultaneous oscillations of the pairs of tubes within the cluster aligned in a perpendicular direction to the incoming wave. However, no signature of a multiple-scattering regime has been observed from this model, while it has been clearly observable for the large compact cluster model. Furthermore, we pointed out the importance of the geometrical shape of the monolithic model on the interaction of f-mode waves with a sunspot in a high-frequency range (ν = 5 mHz). These results are a contribution to the observational effort to distinguish seismically between different configurations of magnetic flux tubes within sunspots and plage.

  19. Seismology of the solar atmosphere

    Science.gov (United States)

    Finsterle, Wolfgang; Jefferies, Stuart M.; Cacciani, Alessandro; Rapex, Paolo; Giebink, Cynthia; Knox, Allister; Dimartino, Vincenzo

    2004-04-01

    We describe a new instrument for seismically probing the properties of the Sun's lower atmosphere, and present some first results from an observational campaign carried out at the geographic South Pole during the austral summer of 2002/2003. A preliminary analysis of the data (simultaneous, high-cadence observations of the velocity signals from the photosphere and low chromosphere) shows that the well-known suppression of acoustic power in regions of strong magnetic field, and enhancement of high-frequency power around active regions (acoustic halos), are both consistent with a spreading out of the magnetic field lines with increasing height in the atmosphere. The data have also revealed some unexpected wave behavior. First, evanescent-like waves are found at frequencies substantially above the acoustic cut-off frequency in regions of intermediate magnetic field. Second, upward- and downward-propagating waves are detected in areas of strong magnetic field such as sunspots and plage: even at frequencies below the acoustic cut-off frequency. Third, the wave behavior in regions of strong magnetic field can change over periods of a few hours from propagating to evanescent. While we have no concrete explanation for the first two results, the latter result opens up the question of whether sound waves are involved in short-term events such as flares or CME's.

  20. Three-dimensional non-LTE radiative transfer effects in Fe I lines I. Flux sheet and flux tube geometries

    CERN Document Server

    Holzreuter, R

    2012-01-01

    In network and active region plages, the magnetic field is concentrated into structures often described as flux tubes (FTs) and sheets (FSs). 3-D radiative transfer (RT) is important for energy transport in these concentrations. It is also expected to be important for diagnostic purposes but has rarely been applied for that purpose. Using true 3-D, non-LTE (NLTE) RT in FT/FS models, we compute Fe line profiles commonly used to diagnose the Sun's magnetic field by comparing the results with those obtained from LTE/1-D (1.5-D) NLTE calculations. Employing a multilevel iron atom, we study the influence of basic parameters such as Wilson depression, wall thickness, radius/width, thermal stratification or magnetic field strength on all Stokes $I$ parameters in the thin-tube approximation. The use of different levels of approximations of RT may lead to considerable differences in profile shapes, intensity contrasts, equivalent widths, and the determination of magnetic field strengths. In particular, LTE, which ofte...

  1. 70 Years of Sunspot Observations at the Kanzelhöhe Observatory: Systematic Study of Parameters Affecting the Derivation of the Relative Sunspot Number

    Science.gov (United States)

    Pötzi, Werner; Veronig, Astrid M.; Temmer, Manuela; Baumgartner, Dietmar J.; Freislich, Heinrich; Strutzmann, Heinz

    2016-03-01

    The Kanzelhöhe Observatory (KSO) was founded during World War II by the Deutsche Luftwaffe (German Airforce) as one station of a network of observatories that were set up to provide information on solar activity in order to better assess the actual conditions of the Earth's ionosphere in terms of radio-wave propagation. Solar observations began in 1943 with photographs of the photosphere and drawings of sunspots, plage regions, and faculae, as well as patrol observations of the solar corona. At the beginning, all data were sent to Freiburg (Germany). After WW II, international cooperation was established and the data were sent to Zurich, Paris, Moscow, and Greenwich. Relative sunspot numbers have been derived since 1944. The agreement between relative sunspot numbers derived at KSO and the new International Sunspot Number (ISN) (SILSO World Data Center in International Sunspot Number Monthly Bulletin and online catalogue, 1945 - 2015) lies within {≈} 10 %. However, revisiting the historical data, we also find periods with larger deviations. The reasons for the deviations were twofold: On the one hand, a major instrumental change took place during which the instrument was relocated and modified. On the other hand, a period of frequent replacements of personnel caused significant deviations; this clearly shows the importance of experienced observers. In the long term, the instrumental improvements led to better image quality. Additionally, we find a long-term trend towards better seeing conditions that began in 2000.

  2. 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.

  3. 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...

  4. First Direct Detection of Magnetic Fields in Starspots and Stellar Chromospheres

    CERN Document Server

    Berdyugina, S V; Afram, N; Suwald, F; Petit, P; Arnaud, J; Harrington, D M; Kuhn, J R

    2007-01-01

    Here we report on the first detection of circular polarization in molecular lines formed in cool magnetic regions (starspots) and in chromospheric emission lines formed in hot plages on the surfaces of active stars. Our survey of G-K-M stars included young main-sequence dwarfs and RS CVn-type giants and subgiants. All stars were found to possess surface magnetic fields producing Stokes V LSD signals in atomic lines of 0.05 to 0.5%. Several stars clearly showed circular polarization in molecular lines of 0.1 to 1%. The molecular Stokes V signal is reminiscent of that observed in sunspots. Chromospheric magnetic fields were detected on most active targets in Stokes V profiles of emission lines with peak polarization up to 2%. The observed molecular circular polarization on M dwarfs indicates single-polarity magnetic fields covering at least 10% of the stellar disk. Smaller signals on K stars imply that their magnetic fields are apparently weaker, more entangled than on M dwarfs, or more diluted by the bright ph...

  5. 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)

  6. Three-dimensional simulations of near-surface convection in main-sequence stars. III. The structure of small-scale magnetic flux concentrations

    CERN Document Server

    Beeck, Benjamin; Cameron, Robert H; Reiners, Ansgar

    2015-01-01

    The convective envelopes of cool main-sequence stars harbour magnetic fields with a complex global and local structure. These fields affect the near-surface convection and the outer stellar atmospheres in many ways and are responsible for the observable magnetic activity of stars. Our aim is to understand the local structure in unipolar regions with moderate average magnetic flux density. These correspond to plage regions covering a substantial fraction of the surface of the Sun (and likely also the surface of other Sun-like stars) during periods of high magnetic activity. We analyse the results of 18 local-box magnetohydrodynamics simulations covering the upper layers of the convection zones and the photospheres of cool main-sequence stars of spectral types F to early M. The average vertical field in these simulations ranges from 20 to 500G. We find a substantial variation of the properties of the surface magnetoconvection between main-sequence stars of different spectral types. As a consequence of a reduced...

  7. The continuum intensity as a function of magnetic field II. Local magnetic flux and convective flows

    CERN Document Server

    Kobel, P; Borrero, J M

    2014-01-01

    To deepen our understanding of the role of small-scale magnetic fields in active regions (ARs) and in the quiet Sun (QS) on the solar irradiance, it is fundamental to investigate the physical processes underlying their continuum brightness. Previous results showed that magnetic elements in the QS reach larger continuum intensities than in ARs at disk center, but left this difference unexplained. We use Hinode/SP disk center data to study the influence of the local amount of magnetic flux on the vigour of the convective flows and the continuum intensity contrasts. The apparent (i.e. averaged over a pixel) longitudinal field strength and line-of-sight (LOS) plasma velocity were retrieved by means of Milne-Eddington inversions (VFISV code). We analyzed a series of boxes taken over AR plages and the QS, to determine how the continuum intensity contrast of magnetic elements, the amplitude of the vertical flows and the box-averaged contrast were affected by the mean longitudinal field strength in the box (which sca...

  8. Chromospheric heating by acoustic waves compared to radiative cooling

    CERN Document Server

    Sobotka, M; Švanda, M; Jurčák, J; del Moro, D; Berrilli, F

    2016-01-01

    Acoustic and magnetoacoustic waves are among the possible candidate mechanisms that heat the upper layers of solar atmosphere. A weak chromospheric plage near a large solar pore NOAA 11005 was observed on October 15, 2008 in the lines Fe I 617.3 nm and Ca II 853.2 nm with the Interferometric Bidimemsional Spectrometer (IBIS) attached to the Dunn Solar Telescope. Analyzing the Ca II observations with spatial and temporal resolutions of 0.4" and 52 s, the energy deposited by acoustic waves is compared with that released by radiative losses. The deposited acoustic flux is estimated from power spectra of Doppler oscillations measured in the Ca II line core. The radiative losses are calculated using a grid of seven 1D hydrostatic semi-empirical model atmospheres. The comparison shows that the spatial correlation of maps of radiative losses and acoustic flux is 72 %. In quiet chromosphere, the contribution of acoustic energy flux to radiative losses is small, only of about 15 %. In active areas with photospheric ma...

  9. STEREO Observations of Quasi-Periodically Driven High Velocity Outflows in Polar Plumes

    CERN Document Server

    McIntosh, Scott W; De Pontieu, Bart; Leamon, Robert J

    2010-01-01

    Plumes are one of the most ubiquitous features seen at the limb in polar coronal holes and are considered to be a source of high density plasma streams to the fast solar wind. We analyze STEREO observations of plumes and aim to reinterpret and place observations with previous generations of EUV imagers within a new context that was recently developed from Hinode observations. We exploit the higher signal-to-noise, spatial and temporal resolution of the EUVI telescopes over that of SOHO/EIT to study the temporal variation of polar plumes in high detail. We employ recently developed insight from imaging (and spectral) diagnostics of active region, plage, and quiet Sun plasmas to identify the presence of apparent motions as high-speed upflows in magnetic regions as opposed to previous interpretations of propagating waves. In almost all polar plumes observed at the limb in these STEREO sequences, in all coronal passbands, we observe high speed jets of plasma traveling along the structures with a mean velocity of ...

  10. Propagation of magnetically guided acoustic shocks in the solar chromosphere

    Science.gov (United States)

    Foukal, P.; Smart, M.

    1981-01-01

    The propagation of a train of acoustic shocks guided by diverging magnetic fields through a static model of the solar chromospheric network and transition region is investigated. For initial flux densities of 1,000,000 ergs/sq cm/sec in the lower chromosphere, the local efficiency of acoustic transmission into the corona can be much higher than that calculated for a plane parallel atmosphere. Acoustic energy will tend to be deposited at higher chromospheric levels in diverging magnetic fields, and magnetic guiding may influence the temperature profile of the network and plages. The total flux that can be transmitted into the corona along such diverging fields is severely limited since the magnetic elements occupy a small fractional area of the photosphere and the transmission efficiency is a rapidly decreasing function of initial flux density. Diverging magnetic fields and a varying ratio of specific heats are not likely to allow high frequency shocks to dissipate high enough in a static atmosphere to contribute significantly to the coronal energy balance.

  11. 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...

  12. On The Magnetic-Field Diagnostics Potential of SDO/HMI

    Science.gov (United States)

    Fleck, Bernard; Hayashi, K.; Rezaei, R.; Vitas, N.; Centeno, R.; Cheung, M.; Couvidat, S.; Fischer, C.; Steiner, O.; Straus, T.; Viticchie, B.

    2012-05-01

    The Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) is designed to study oscillations and the magnetic field in the solar photosphere. It observes the full solar disk in the Fe I absorption line at 6173 Å. We use the output of three high-resolution 3D, time-dependent, radiative magneto-hydrodynamics simulations (two based on the MURaM code, one on the CO5BOLD code) to calculate Stokes profiles for the Fe I 6173 Å line for snapshots of a sunspot, a plage area and an enhanced network region. Stokes filtergrams are constructed for the 6 nominal HMI wavelengths by multiplying the Stokes profiles with a representative set of HMI filter response functions. The magnetic field vector B(x,y) and line-of-sight Doppler velocities V(x,y) are determined from these filtergrams using a simplified version of the HMI magnetic field processing pipeline. Finally, the reconstructed magnetic field B(x,y) and line-of-sight velocity V(x,y) are compared to the actual magnetic field B0(x,y,z) and vertical velocity V0(x,y,z) in the simulations.

  13. 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.

  14. Disentangling stellar activity and planetary signals

    Directory of Open Access Journals (Sweden)

    Santos N.C.

    2011-02-01

    Full Text Available Photospheric stellar activity (i.e. dark spots or bright plages might be an important source of noise and confusion in the radial-velocity (RV measurements. Radial-velocimetry planet search surveys as well as follow-up of photometric transit surveys require a deep understanding and precise characterization of the effects of stellar activity, in order to disentangle it from planetary signals. We simulate dark spots on a rotating stellar photosphere. The variations of the RV are characterized and analyzed according to the stellar inclination, the latitude and the number of spots. The Lomb-Scargle periodograms of the RV variations induced by activity present power at the rotational period Prot of the star and its two-first harmonics Prot/2 and Prot/3. Three adjusted sinusoids fixed at the fundamental period and its two-first harmonics allow to remove about 90% of the RV jitter amplitude. We apply and validate our approach on four known active planet-host stars: HD 189733, GJ 674, CoRoT-7 and ι Hor.

  15. 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.

  16. 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.

  17. Late-glacial to Early Holocene lake basin and river valley formation within Pomeranian moraine belt near Dobbertin (Mecklenburg-Vorpommern, NE Germany)

    Science.gov (United States)

    Zawiska, Izabela; Lorenz, Sebastian; Börner, Andreas; Niessner, Dominique; Słowiński, Michał; Theuerkauf, Martin; Pieper, Hagen; Lampe, Reinhard

    2014-05-01

    related to a cold period with permafrost formation. At other positions in the basin, the basal peat layer is covered directly by calcareous and silicate gyttias. These parts may (1) either not have been affected by assumed fluvial activity or (2) peat formation as such only started later here. Finally, an extended lake filled the basin from the later parts of the late-glacial on. Its sedimentation history is well recorded in calcareous and silicate gyttjas, whereas sedimentary units derived from organic and inorganic carbon content as well as grain size distribution allows a stratigraphical comparison of different profiles. Several delta cones in lake sediments give evidence of still considerable fluvial influx. High lake levels are indicated by lake terraces at 51 m and 43 m a.s.l., yet the timing of these high stands is still unclear. A third terrace at 41 m a.s.l. represents lower water level in historic times, during which two smaller lakes ('Dobbiner Plage' and 'Klädener Plage') existed in the basin. Both lakes vanished due to drainage after 1798. The uppermost sediment sequence in the basins is represented by a pattern of strongly decomposed peat and lacustrine sand.

  18. 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

  19. 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

  20. Etude du stockage de l'hydrogene sur des nanostructures de carbone microporeuses

    Science.gov (United States)

    Poirier, Eric

    2007-12-01

    Le stockage de l'hydrogene par adsorption sur des adsorbants nano-structures a ete etudie sous differentes conditions de pression et de temperature. Les adsorbants etudies sont principalement des nanotubes de carbone a simple paroi ainsi que des structures metallo-organiques. Les mesures ont ete realisees a l'aide de systemes gravimetriques et volumetriques tres sensibles specialement mis au point pour de petits echantillons necessitant un degazage in situ. Les appareils developpes, au nombre de quatre, comprennent deux systemes gravimetriques et deux systemes volumetriques. Ensemble, ces systemes couvrent la plage de pressions (0-100) bars ainsi que la plage de temperatures (77-295) K. Les differentes analyses montrent que l'adsorption d'hydrogene sur les adsorbants nano-structures etudies est maximale a 77 K et varie entre environ (1.5 et 4) % masse. A temperature ambiante, l'adsorption croit lineairement avec la pression et demeure sous les 1% masse pour des pressions inferieures a 100 bars. L'adsorption d'hydrogene sur ces materiaux dans ces conditions se compare notamment a celle obtenue sur des charbons actives. La modelisation de l'adsorption a egalement ete realisee dans des conditions cryogeniques a l'aide du modele de Dubinin-Astakhov sous une forme adaptee pour l'adsorption supercritique. Les enthalpies d'adsorption calculees a partir de ce modele varient sous les 6 kJ/mole et sont donc consistantes avec des processus de physisorption. L'applicabilite du modele de Dubinin-Astakhov suggere que l'adsorption d'hydrogene puisse etre representee par un processus de remplissage des pores par un pseudo-liquide. Ces travaux s'inscrivent dans un contexte ou la capacite d'adsorption reelle des nanostructures de carbone est sujette a la controverse. En consequence, l'approche experimentale adoptee se distingue par les differentes demarches mises de l'avant pour l'obtention de mesures fiables sur des echantillons de faibles masses ainsi que par son caractere

  1. Density diagnostics derived from the O iv and S iv intercombination lines observed by IRIS

    Science.gov (United States)

    Polito, V.; Del Zanna, G.; Dudík, J.; Mason, H. E.; Giunta, A.; Reeves, K. K.

    2016-10-01

    The intensity of the O iv 2s2 2p 2P-2s2p24P and S iv 3 s2 3p 2P-3s 3p24 P intercombination lines around 1400 Å observed with the Interface Region Imaging Spectrograph (IRIS) provide a useful tool to diagnose the electron number density (Ne) in the solar transition region plasma. We measure the electron number density in a variety of solar features observed by IRIS, including an active region (AR) loop, plage and brightening, and the ribbon of the 22-June-2015 M 6.5 class flare. By using the emissivity ratios of O iv and S iv lines, we find that our observations are consistent with the emitting plasma being near isothermal (logT[K] ≈ 5) and iso-density (Ne ≈ 1010.6 cm-3) in the AR loop. Moreover, high electron number densities (Ne ≈ 1013 cm-3) are obtained during the impulsive phase of the flare by using the S iv line ratio. We note that the S iv lines provide a higher range of density sensitivity than the O iv lines. Finally, we investigate the effects of high densities (Ne ≳ 1011 cm-3) on the ionization balance. In particular, the fractional ion abundances are found to be shifted towards lower temperatures for high densities compared to the low density case. We also explored the effects of a non-Maxwellian electron distribution on our diagnostic method. The movie associated to Fig. 3 is available at http://www.aanda.org

  2. Magnetic activity in the young solar analog LQ Hydrae. I. Active longitudes and cycles

    Science.gov (United States)

    Berdyugina, S. V.; Pelt, J.; Tuominen, I.

    2002-11-01

    We present the first evidence that a single active dwarf of solar type can show a long-lived, nonaxisymmetric spot distribution - active longitudes on opposite hemispheres, similar to evolved, rapidly rotating RS CVn-type binary stars. We analyse new as well as published photometric observations of the young active dwarf LQ Hya, spanning almost 20 years. We find that activity of the star has three activity cycles: a 5.2-yr ``flip-flop'' cycle, a 7.7-yr period in the amplitude modulation of the brightness and an approximately 15-yr period in variations of the mean brightness. The two shorter cycles are related to the alternating active longitudes and are similar to cycles observed in RS CVn-type stars. The 15-yr cycle reflects periodic changes of the mean spottedness of the star and resembles the solar 11-year cycle. The spot rotation period (about 1.6 days) changes during the 15-yr cycle, indicating the presence of small differential rotation. The lengths of the three cycles are related as 3:2:1, with the repetition of the spot configuration after 15 years. We discuss the possibility that the observed spot cycles represent two different magnetic dynamo modes operating in LQ Hya: an axisymmetric mode, as in the Sun, and a nonaxisymmetric higher order mode with two cycles in spot patterns. Our results suggest that young stars exhibit their cycles in spot distribution, as seen in LQ Hya. This is in contrast to the conclusion based on the analysis of Ca Ii H&K emission from plages. The results suggest also that the Vaughan-Preston gap represents a transition from a multiple-mode dynamo to a single-mode dynamo. Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/394/505

  3. Comparison of Far-side Helioseismic Predictions of Active Regions from SDO/HMI with Far-side Observations of Solar Activity from STEREO/EUVI

    Science.gov (United States)

    Liewer, Paulett C.; Qiu, Jiong; Charles, Lindsey

    2017-08-01

    Doppler data from the Helioseismic and Magnetic Imager (HMI) aboard the Solar Dynamics Observatory (SDO) are now being used routinely to detect strong magnetic field regions on the far side of the Sun (http:/jsoc.stanford.edu/data/farside/). To test the reliability of these active regions predictions, the far-side seismic region detections are compared with far-side observation of solar activity from the Solar TErrestrial RElations Observatory (STEREO), using brightness in extreme ultraviolet light as a proxy for strong magnetic fields. Two approaches are used here to compare and analyze approximately six months of STEREO and HMI data. In the first approach, after determining whether or not new large East-limb active regions were detected seismically on the far side of the Sun before they appeared Earth side, we analyze how the ability to detect these regions seismically relates to their integrated extreme ultraviolet intensity. We find that, while there is a range of intensities where far-side regions may or may not be detected seismically, there appears to be an intensity level above which they are always detected and an intensity level below which they are never detected. In the second approach, we analyze concurrent extreme ultraviolet and helioseismic far-side maps for the same six month period. We find that 100% (22) of the far-side seismic regions correspond to an extreme ultraviolet plage; 95% of these either became a NOAA-designated magnetic region when reaching the east limb or were one before crossing to the far side. A low but significant correlation is found between the seismic signature strength and the EUV intensity of a far-side region.

  4. Measurements of Photospheric and Chromospheric Magnetic Fields

    Science.gov (United States)

    Lagg, Andreas; Lites, Bruce; Harvey, Jack; Gosain, Sanjay; Centeno, Rebecca

    2017-09-01

    The Sun is replete with magnetic fields, with sunspots, pores and plage regions being their most prominent representatives on the solar surface. But even far away from these active regions, magnetic fields are ubiquitous. To a large extent, their importance for the thermodynamics in the solar photosphere is determined by the total magnetic flux. Whereas in low-flux quiet Sun regions, magnetic structures are shuffled around by the motion of granules, the high-flux areas like sunspots or pores effectively suppress convection, leading to a temperature decrease of up to 3000 K. The importance of magnetic fields to the conditions in higher atmospheric layers, the chromosphere and corona, is indisputable. Magnetic fields in both active and quiet regions are the main coupling agent between the outer layers of the solar atmosphere, and are therefore not only involved in the structuring of these layers, but also for the transport of energy from the solar surface through the corona to the interplanetary space. Consequently, inference of magnetic fields in the photosphere, and especially in the chromosphere, is crucial to deepen our understanding not only for solar phenomena such as chromospheric and coronal heating, flares or coronal mass ejections, but also for fundamental physical topics like dynamo theory or atomic physics. In this review, we present an overview of significant advances during the last decades in measurement techniques, analysis methods, and the availability of observatories, together with some selected results. We discuss the problems of determining magnetic fields at smallest spatial scales, connected with increasing demands on polarimetric sensitivity and temporal resolution, and highlight some promising future developments for their solution.

  5. Three-dimensional mapping of fine structure in the solar atmosphere

    Science.gov (United States)

    Henriques, Vasco M. J.

    2013-04-01

    The effects on image formation through a tilted interference filter in a converging beam are investigated and an adequate compensation procedure is established. A method that compensates for small-scale seeing distortions is also developed with the aim of co-aligning non-simultaneous solar images from different passbands. These techniques are applied to data acquired with a narrow tiltable filter at the Swedish 1-meter Solar Telescope. Tilting provides a way to scan the wing of the Ca II H line. The resulting images are used to map the temperature stratification and vertical temperature gradients in a solar active region containing a sunspot at a resolution approaching 0''10. The data are compared with hydro-dynamical quiet sun models and magneto-hydrodynamic models of plage. The comparison gives credence to the observational techniques, the analysis methods, and the simulations. Vertical temperature gradients are lower in magnetic structures than in non-magnetic. Line-of-sight velocities and magnetic field properties in the penumbra of the same sunspot are estimated using the CRISP imaging spectropolarimeter and straylight compensation adequate for the data. These reveal a pattern of upflows and downflows throughout the entire penumbra including the interior penumbra. A correlation with intensity positively identifies these flows as convective in origin. The vertical convective signatures are observed everywhere, but the horizontal Evershed flow is observed to be confined to areas of nearly horizontal magnetic field. The relation between temperature gradient and total circular polarization in magnetically sensitive lines is investigated in different structures of the penumbra. Penumbral dark cores are prominent in total circular polarization and temperature gradient maps. These become longer and more contiguous with increasing height. Dark fibril structures over bright regions are observed in the Ca II H line core, above both the umbra and penumbra.

  6. Magnetic Flux Emergence Observed with the Advanced Stokes Polarimeter

    Science.gov (United States)

    Lites, B.; Martinez Pillet, V.

    1996-05-01

    We have carried out quantitative observations of the vector magnetic field during the emergence of three small bipolar active regions in June, 1992, July 1993, and September 1994 using the Advanced Stokes Polarimeter (ASP). The region of horizontal magnetic field at the actual site of emergence is always characterized by low magnetic field strength (i.e. considerably less than 1000 Gauss). We find a strong relationship between field strength and inclination in these regions. This suggests that 1) flux emerging from below the photosphere does not coalesce into strong flux tubes until it reaches the photosphere, becomes nearly vertical as a result of magnetic buoyancy, and is then acted upon by convective collapse, and 2) the field strength of flux rising through the convection zone may be in rough equipartition with the fluid motions. We find the flux emergence zone to be characterized by highly variable (both spatially and temporally) fill factors for the magnetic field, suggesting that the flux below the surface is filamentary, that it rises rapidly through the photosphere to form a magnetic canopy above the emergence region. Sequences of Hα on- and off-band images obtained with the ASP reveal the accompanying development of the arch-filament system, and suggest that the material within the Hα structures is supplied by a siphon flow as evidenced by apparent chromospheric red shifts on the sides of the loops closest to a large pore, and blue shifts where the fields anchor in plage regions. Proper motions of the magnetic flux images throughout a day's observation indicate the presence of a persistent vortex flow on a small scale (a few arcseconds). The National Center for Atmospheric Research is sponsored by the National Science Foundation.

  7. Ca II 854.2 nm Spectromagnetograms: A Powerful Chromospheric Diagnostic

    Science.gov (United States)

    Harvey, J. W.; Bertello, Luca; Branston, D.; Britanik, J.; Bulau, S.; Cole, L.; Gosain, Sanjay; Harker, Brian; Jones, Harrison P.; Marble, A.; Martinez Pillet, V.; Pevtsov, A.; Schramm, K.; Streander, Kim; Villegas, H.

    2016-05-01

    The transition from physical dominance by plasma flows in the photosphere to magnetic pressure in the solar chromosphere motivates as many diagnostic observations as possible across this important region. Among the few ground-accessible spectral lines formed within the chromosphere, the Ca II 854.2 nm line has the desirable properties of presence everywhere on the solar disk, Zeeman sensitivity, and narrow line width. Mapped observations of circular polarization within this line (spectromagnetograms) have been made at NSO infrequently since 1974, with regular daily full-disk observations starting in August 1996. Full-disk spectral observations of the complete Stokes polarization vector are now being made regularly since November 2015. It is not easy to estimate chromospheric magnetic field properties from the 854.2 nm line profile polarization. To provide rough quick-look vector field maps we found that the weak-field approximation provides a fair first estimate of the line-of-sight component but appears to be too simple to interpret the transverse magnetic field from frequently asymmetric, linearly-polarized line profiles. More realistic estimates of the chromospheric vector field, short of extremely lengthy, full 3D, non-local radiative transfer inversions, are being investigated. We briefly introduce recent instrumental modifications and observational characteristics, sample observations, and results concerning the expansion of the chromospheric field with increasing height, the presence of large areas of weak, nearly horizontal fields, and field estimates in plages, sunspots, flares, filaments, and filament channels. The Stokes spectra will be freely available to the community.This work utilizes SOLIS data obtained by the NSO Integrated Synoptic Program (NISP), managed by the National Solar Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation.

  8. 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.

  9. Solar Indices Forecasting Tool

    Science.gov (United States)

    Henney, Carl John; Shurkin, Kathleen; Arge, Charles; Hill, Frank

    2016-05-01

    Progress to forecast key space weather parameters using SIFT (Solar Indices Forecasting Tool) with the ADAPT (Air Force Data Assimilative Photospheric flux Transport) model is highlighted in this presentation. Using a magnetic flux transport model, ADAPT, we estimate the solar near-side field distribution that is used as input into empirical models for predicting F10.7(solar 10.7 cm, 2.8 GHz, radio flux), the Mg II core-to-wing ratio, and selected bands of solar far ultraviolet (FUV) and extreme ultraviolet (EUV) irradiance. Input to the ADAPT model includes the inferred photospheric magnetic field from the NISP ground-based instruments, GONG & VSM. Besides a status update regarding ADAPT and SIFT models, we will summarize the findings that: 1) the sum of the absolute value of strong magnetic fields, associated with sunspots, is shown to correlate well with the observed daily F10.7 variability (Henney et al. 2012); and 2) the sum of the absolute value of weak magnetic fields, associated with plage regions, is shown to correlate well with EUV and FUV irradiance variability (Henney et al. 2015). This work utilizes data produced collaboratively between Air Force Research Laboratory (AFRL) and the National Solar Observatory (NSO). The ADAPT model development is supported by AFRL. The input data utilized by ADAPT is obtained by NISP (NSO Integrated Synoptic Program). NSO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation (NSF). The 10.7 cm solar radio flux data service, utilized by the ADAPT/SIFT F10.7 forecasting model, is operated by the National Research Council of Canada and National Resources Canada, with the support of the Canadian Space Agency.

  10. North-south asymmetry of Ca II K regions determined from OAUC spectroheliograms: 1996 - 2006

    Science.gov (United States)

    Dorotovič, I.; Rybák, J.; Garcia, A.; Journoud, P.

    2010-12-01

    The solar activity (SA) evolution levels are not identical in the northern and southern Sun's hemispheres. This fact was repeatedly confirmed in the past by the analysis of a number of long-term observations of various SA indices in individual atmospheric layers of the Sun and in different bandwidths. The north-south asymmetry (NSA) is thus a significant tool in investigation of long-term SA variations. This paper presents a software tool to determine the NSA of the area of bright chromospheric plages, as measured in the Ca II K3 spectroheliograms registered since 1926 in the Observatário Astronómico da Universidade de Coimbra, Portugal, as well as evolution of sizes of these areas in the period 1996 - 2006. The algorithm of the program is limited to determining the total area of bright features in the Ca II K3 emission line based on the definition of the threshold value for relative brightness and, therefore, it does not resolve brightness of individual chromospheric features. A comparison and cross-correlation of this NSA with the NSAs found for the sunspots and coronal green line brightness have been added. In the near future we intend to 1) determine the NSA of the area of bright chromospheric Ca II K3 regions back to the year 1926, and 2) compare the evolution of the surface area of these regions in the period 1970-2006 with the evolution of the magnetic index obtained at Mt. Wilson Observatory, which would also help in setting up a proxy reconstruction of the magnetic index back to 1926. Since 2007 new spectroheliograms have been recorded using a CCD camera and, therefore, in the future we will also address this issue for the period 2007 - present.

  11. 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.

  12. ULTRAVIOLET SPECTROSCOPY OF RAPIDLY ROTATING SOLAR-MASS STARS: EMISSION-LINE REDSHIFTS AS A TEST OF THE SOLAR-STELLAR CONNECTION

    Energy Technology Data Exchange (ETDEWEB)

    Linsky, Jeffrey L. [JILA, University of Colorado and NIST, 440UCB Boulder, CO 80309-0440 (United States); Bushinsky, Rachel [APS, University of Colorado, 391UCB Boulder, CO 80309-0391 (United States); Ayres, Tom; France, Kevin, E-mail: jlinsky@jilau1.colorado.edu [CASA, University of Colorado, 593UCB Boulder, CO 80309-0593 (United States)

    2012-07-20

    We compare high-resolution ultraviolet spectra of the Sun and thirteen solar-mass main-sequence stars with different rotational periods that serve as proxies for their different ages and magnetic field structures. In this, the second paper in the series, we study the dependence of ultraviolet emission-line centroid velocities on stellar rotation period, as rotation rates decrease from that of the Pleiades star HII314 (P{sub rot} = 1.47 days) to {alpha} Cen A (P{sub rot} = 28 days). Our stellar sample of F9 V to G5 V stars consists of six stars observed with the Cosmic Origins Spectrograph on the Hubble Space Telescope (HST) and eight stars observed with the Space Telescope Imaging Spectrograph on HST. We find a systematic trend of increasing redshift with more rapid rotation (decreasing rotation period) that is similar to the increase in line redshift between quiet and plage regions on the Sun. The fastest-rotating solar-mass star in our study, HII314, shows significantly enhanced redshifts at all temperatures above log T = 4.6, including the corona, which is very different from the redshift pattern observed in the more slowly rotating stars. This difference in the redshift pattern suggests that a qualitative change in the magnetic-heating process occurs near P{sub rot} = 2 days. We propose that HII314 is an example of a solar-mass star with a magnetic heating rate too large for the physical processes responsible for the redshift pattern to operate in the same way as for the more slowly rotating stars. HII314 may therefore lie above the high activity end of the set of solar-like phenomena that is often called the 'solar-stellar connection'.

  13. LOFAR tied-array imaging and spectroscopy of solar S bursts

    Science.gov (United States)

    Morosan, D. E.; Gallagher, P. T.; Zucca, P.; O'Flannagain, A.; Fallows, R.; Reid, H.; Magdalenić, J.; Mann, G.; Bisi, M. M.; Kerdraon, A.; Konovalenko, A. A.; MacKinnon, A. L.; Rucker, H. O.; Thidé, B.; Vocks, C.; Alexov, A.; Anderson, J.; Asgekar, A.; Avruch, I. M.; Bentum, M. J.; Bernardi, G.; Bonafede, A.; Breitling, F.; Broderick, J. W.; Brouw, W. N.; Butcher, H. R.; Ciardi, B.; de Geus, E.; Eislöffel, J.; Falcke, H.; Frieswijk, W.; Garrett, M. A.; Grießmeier, J.; Gunst, A. W.; Hessels, J. W. T.; Hoeft, M.; Karastergiou, A.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; McKay-Bukowski, D.; McKean, J. P.; Munk, H.; Orru, E.; Paas, H.; Pizzo, R.; Polatidis, A. G.; Scaife, A. M. M.; Sluman, J.; Tasse, C.; Toribio, M. C.; Vermeulen, R.; Zarka, P.

    2015-08-01

    Context. The Sun is an active source of radio emission that is often associated with energetic phenomena ranging from nanoflares to coronal mass ejections (CMEs). At low radio frequencies (<100 MHz), numerous millisecond duration radio bursts have been reported, such as radio spikes or solar S bursts (where S stands for short). To date, these have neither been studied extensively nor imaged because of the instrumental limitations of previous radio telescopes. Aims: Here, LOw Frequency ARray (LOFAR) observations were used to study the spectral and spatial characteristics of a multitude of S bursts, as well as their origin and possible emission mechanisms. Methods: We used 170 simultaneous tied-array beams for spectroscopy and imaging of S bursts. Since S bursts have short timescales and fine frequency structures, high cadence (~50 ms) tied-array images were used instead of standard interferometric imaging, that is currently limited to one image per second. Results: On 9 July 2013, over 3000 S bursts were observed over a time period of ~8 h. S bursts were found to appear as groups of short-lived (<1 s) and narrow-bandwidth (~2.5 MHz) features, the majority drifting at ~3.5 MHz s-1 and a wide range of circular polarisation degrees (2-8 times more polarised than the accompanying Type III bursts). Extrapolation of the photospheric magnetic field using the potential field source surface (PFSS) model suggests that S bursts are associated with a trans-equatorial loop system that connects an active region in the southern hemisphere to a bipolar region of plage in the northern hemisphere. Conclusions: We have identified polarised, short-lived solar radio bursts that have never been imaged before. They are observed at a height and frequency range where plasma emission is the dominant emission mechanism, however, they possess some of the characteristics of electron-cyclotron maser emission. A movie associated to Fig. 3 is available in electronic form at http://www.aanda.org

  14. Processes and rate of retreat of the clay and sandstone sea cliffs of the northern Boulonnais (France)

    Science.gov (United States)

    Pierre, Guillaume

    2006-01-01

    Retreat of the clay and sandstone cliffs of the northern Boulonnais (France) has been quantified using stereophotogrammetry. The low retreat rate of this coastal strip — 0.08 m/yr between 1939 and 2003 — is far less than that encountered on chalk and clay-chalk cliffs of either side of the Channel, and even less than a previous estimate of 0.17 m/yr regularly quoted in management studies. The retreat rate is closely related to shore platform morphology and dynamics. The shore platform presents 1) a steeply sloping ramp due to the accumulation of flat calcareous megaclasts that reduce marine erosion; 2) upstanding bare platform surfaces, related to tectonic deformation; and 3) thick platform-beaches trapped in troughs. In all three cases, the reflective behaviour of the nearshore protects the cliff foot from the incoming waves. Two critical eroding segments are the result of changes in the platform sedimentary budget. Around Cran Poulet, and between Plage de la Sirène and Pointe de la Courte Dune, the retreat rate is up to 0.25 and 0.15 m/yr, respectively. At Cran Poulet, recession has been facilitated by the extraction of pebble for more than half a century, whereas erosion of the beach at la Sirène is probably linked to severe erosion of the coastline in the adjacent Wissant Bay. Mass movements on the cliff face are essentially shallow-seated translational slides along with small debris falls and mudflows. The instability of the Argiles de Châtillon is greatly diminished by their sandy and silty texture and by the presence of interstratified solid shelly limestone beds that allow steep slopes to develop in rather weak material. The 'vertical erosion antecedent' is the erosional mode of the cliff, and its reduced efficiency explains the slow recession of the cliff. This study will help to determine the long term evolution of the Boulonnais coast.

  15. Etude de la dynamique des porteurs dans des nanofils de silicium par spectroscopie terahertz

    Science.gov (United States)

    Beaudoin, Alexandre

    Ce memoire presente une etude des proprietes de conduction electrique et de la dynamique temporelle des porteurs de charges dans des nanofils de silicium sondes par rayonnement terahertz. Les cas de nanofils de silicium non intentionnellement dopes et dopes type n sont compares pour differentes configurations du montage experimental. Les mesures de spectroscopie terahertz en transmission montre qu'il est possible de detecter la presence de dopants dans les nanofils via leur absorption du rayonnement terahertz (˜ 1--12 meV). Les difficultes de modelisation de la transmission d'une impulsion electromagnetique dans un systeme de nanofils sont egalement discutees. La detection differentielle, une modification au systeme de spectroscopie terahertz, est testee et ses performances sont comparees au montage de caracterisation standard. Les instructions et des recommendations pour la mise en place de ce type de mesure sont incluses. Les resultats d'une experience de pompe optique-sonde terahertz sont egalement presentes. Dans cette experience, les porteurs de charge temporairement crees suite a l'absorption de la pompe optique (lambda ˜ 800 nm) dans les nanofils (les photoporteurs) s'ajoutent aux porteurs initialement presents et augmentent done l'absorption du rayonnement terahertz. Premierement, l'anisotropie de l'absorption terahertz et de la pompe optique par les nanofils est demontree. Deuxiemement, le temps de recombinaison des photoporteurs est etudie en fonction du nombre de photoporteurs injectes. Une hypothese expliquant les comportements observes pour les nanofils non-dopes et dopes-n est presentee. Troisiemement, la photoconductivite est extraite pour les nanofils non-dopes et dopes-n sur une plage de 0.5 a 2 THz. Un lissage sur la photoconductivite permet d'estimer le nombre de dopants dans les nanofils dopes-n. Mots-cles: nanofil, silicium, terahertz, conductivite, spectroscopie, photoconductivite.

  16. Comparison of Helioseismic Far-Side Active Region Detections with STEREO Far-Side EUV Observations of Solar Activity

    Science.gov (United States)

    Liewer, P. C.; Qiu, J.; Lindsey, C.

    2017-10-01

    Seismic maps of the Sun's far hemisphere, computed from Doppler data from the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) are now being used routinely to detect strong magnetic regions on the far side of the Sun (http://jsoc.stanford.edu/data/farside/). To test the reliability of this technique, the helioseismically inferred active region detections are compared with far-side observations of solar activity from the Solar TErrestrial RElations Observatory (STEREO), using brightness in extreme-ultraviolet light (EUV) as a proxy for magnetic fields. Two approaches are used to analyze nine months of STEREO and HMI data. In the first approach, we determine whether new large east-limb active regions are detected seismically on the far side before they appear Earth side and study how the detectability of these regions relates to their EUV intensity. We find that while there is a range of EUV intensities for which far-side regions may or may not be detected seismically, there appears to be an intensity level above which they are almost always detected and an intensity level below which they are never detected. In the second approach, we analyze concurrent extreme-ultraviolet and helioseismic far-side observations. We find that 100% (22) of the far-side seismic regions correspond to an extreme-ultraviolet plage; 95% of these either became a NOAA-designated magnetic region when reaching the east limb or were one before crossing to the far side. A low but significant correlation is found between the seismic signature strength and the EUV intensity of a far-side region.

  17. Adsorption de gaz sur les materiaux microporeux modelisation, thermodynamique et applications

    Science.gov (United States)

    Richard, Marc-Andre

    2009-12-01

    Nos travaux sur l'adsorption de gaz dans les materiaux microporeux s'inscrivent dans le cadre des recherches visant a augmenter l'efficacite du stockage de l'hydrogene a bord des vehicules. Notre objectif etait d'etudier la possibilite d'utiliser l'adsorption afin d'ameliorer l'efficacite de la liquefaction de l'hydrogene des systemes a petite echelle. Nous avons egalement evalue les performances d'un systeme de stockage cryogenique de l'hydrogene base sur la physisorption. Comme nous avons affaire a des plages de temperatures particulierement etendues et a de hautes pressions dans la region supercritique du gaz, nous avons du commencer par travailler sur la modelisation et la thermodynamique de l'adsorption. La representation de la quantite de gaz adsorbee en fonction de la temperature et de la pression par un modele semi-empirique est un outil utile pour determiner la masse de gaz adsorbee dans un systeme mais egalement pour calculer les effets thermiques lies a l'adsorption. Nous avons adapte le modele Dubinin-Astakhov (D-A) pour modeliser des isothermes d'adsorption d'hydrogene, d'azote et de methane sur du charbon actif a haute pression et sur une grande plage de temperatures supercritiques en considerant un volume d'adsorption invariant. Avec cinq parametres de regression (incluant le volume d'adsorption Va), le modele que nous avons developpe permet de tres bien representer des isothermes experimentales d'adsorption d'hydrogene (de 30 a 293 K, jusqu'a 6 MPa), d'azote (de 93 a 298 K, jusqu'a 6 MPa) et de methane (de 243 a 333 K, jusqu'a 9 MPa) sur le charbon actif. Nous avons calcule l'energie interne de la phase adsorbee a partir du modele en nous servant de la thermodynamique des solutions sans negliger le volume d'adsorption. Par la suite, nous avons presente les equations de conservation de la niasse et de l'energie pour un systeme d'adsorption et valide notre demarche en comparant des simulations et des tests d'adsorption et de desorption. En plus de l

  18. Transitioning GONG data processing to NOAA SWPC operations

    Science.gov (United States)

    Reinard, Alysha; Marble, Andrew R.; Berger, Thomas

    2016-05-01

    The NOAA Space Weather Prediction Center (SWPC) is the nation's official source of space weather watches, warnings, and alerts, providing 24x7 forecasting and support to critical infrastructure operators around the world. Observations of the conditions on the Sun are crucial for determining when and if a warning is needed. The Global Oscillation Network Group (GONG) operated by the National Solar Observatory (NSO) consists of six ground stations, allowing continuous observations of the Sun. Of particular interest for space weather purposes are the H-alpha images and magnetograms. The H-alpha data are used to identify filaments and their eruptions, to assess active region evolution and plage extent, and to help localize flare locations. The magnetograms are used to identify neutral lines, to examine potential shearing areas and to characterize the magnetic structure of active regions. GONG magnetograms also provide the initial condition for models of solar wind expansion through the heliosphere such as the WSA-Enlil model. Although beyond the scope of current space weather applications, GONG helioseismology products can be used to assess active region emergence on the far side of the Sun and to indicate the flaring potential of a front-side active region. These products are being examined as future tools in flare prediction.NSO has operated GONG as a science facility since 1995 and has provided processed space weather data products to NOAA via for the past several years. In 2014 the White House Office of Management and Budget (OMB) requested that NOAA transition the GONG network to an operational space weather asset in order to ensure the continued flow of critical data for solar wind models. NSO will continue to operate and manage the instruments and sites, but the H-alpha images and 10 minute averaged magnetogram data will be sent directly to SWPC for processing and use in space weather modeling. SWPC will make these data available to NSO and the public via the

  19. Re-establishment of Carabus (Cathoplius) aliai Escalera, 1944 as a separate valid species (Coleoptera, Carabidae).

    Science.gov (United States)

    Ghittino, Claudio; Busato, Enrico; Casale, Achille

    2015-01-01

    failure in Carabusaliai × Carabusstenocephalusifniensis hybrids, clearly indicate that Carabusaliai is a separate Cathoplius species that is distributed in an area south of the Anti-Atlas chain, from Plage Blanche (Guelmim) to Lemsid and Bou Kra (south of Laâyoune). Carabusaliai is therefore both a Saharan desert endemic and an Atlantic resident. Moreover, it is the southernmost Carabus species of the western Palaearctic region.

  20. Radiographie par rayons X à haute résolution de défauts topologiques en volume de structures modulées comparée aux neutrons en faisceau blanc

    Science.gov (United States)

    Fernandez Palacio, J.; Hamelin, B.; Marmeggi, J. C.

    2004-11-01

    Une émission de rayons X par un générateur à haute tension (plage : 50 - 410 kV) a été développée pour être utilisée avec un diffractomètre à rayons X durs et caractériser en volume des monocristaux. Le fort flux issu d'une installation de radiologie à foyer fin avec un grand pouvoir de pénétration en profondeur autorise l'étude d'échantillons très absorbants. Quelques exemples de l'utilisation de ces propriétés pour des échantillons épais et très absorbants sont présentés ; principalement l'analyse de contraintes et la topographie X projetée 2D dans des matériaux en comparaison avec l'information par la diffraction des neutrons. La diffraction à haute énergie apparaît dans la direction transmise, les angles de Bragg sont petits et ainsi les différentes lignes de réflexions sont réparties autour du faisceau principal. La presse uni-axiale utilisée pour les expériences est optimisée effectivement avec l'absence d'un bruit de fond dû à l'usage de fentes. L'optique des rayons X durs et neutrons appliquée aux échantillons épais donne une information complémentaire dans les expériences sur l'analyse de la densité volumétrique par la diffusion des rayons X et neutrons. On l'applique à des problèmes concernant des cristaux aux structures modulées étudiées sous des charges mécaniques et thermiques.

  1. Basic research in solar physics

    Science.gov (United States)

    Linsky, Jeffrey L.

    1991-01-01

    This grant, dating back more than 20 years has supported a variety of investigations of the chromospheres and coronae of the Sun and related cool stars by the Principal Investigator, his postdocs and graduate students, and colleagues at other institutions. This work involved studies of radiative transfer and spectral line formation theory, and the application of these techniques to the analysis of spectra obtained from space and ground-based observatories in the optical, ultraviolet, x-ray and radio portions of the spectrum. Space observations have included the analysis of spectra from OSO-7, Skylab, SMM, and the HRTS rocket experiments. Recent work has concentrated on the interaction of magnetic fields, plasma and radiation in the outer atmospheres of the Sun and other magnetically active stars with different fundamental parameters. Our study of phenomena common to the Sun and stars, the 'solar-stellar connection', can elucidate the fundamental physics, because spatially-resolved observations of the Sun provide us with the 'groundtruth,' while interpretation of stellar data permit us to isolate those parameters critical to stellar activity. Recently, we have studied the differences in physical properties between solar regions of high magnetic flux density and the surrounding plasma. High-resolution CN and CO spectroheliograms have been used to model the thermal inhomogeneities driven by unstable CO cooling, and we have analyzed spatially resolved UV spectra from HRTS to model the thermal structure and energy balance of small-scale structures. The study of nonlinear relations between atmospheric radiative losses and the photospheric magnetic flux density has been continued. We have also proposed a new model for the decay of plages by random walk diffusion of magnetic flux. Our analysis of phenomena common to the Sun and stars included the application of available spectroscopic diagnostics, establishing evidence that the atmospheres of the least active stars are

  2. Exploring the optical contrast effect in strong atomic lines for exoplanets transiting active stars

    Science.gov (United States)

    Cauley, Paul W.; Redfield, Seth

    2017-01-01

    Transmission spectroscopy is a powerful tool for detecting and characterizing planetary atmospheres. Non-photospheric features on the stellar disk, however, can contaminate the planetary signal: during transit the observed spectrum is weighted towards the features not currently being occulted by the planet. This contrast effect can mimic absorption in the planetary atmosphere for strong atomic lines such as Na I, Ca II, and the hydrogen Balmer lines. While the contrast effect is negligible for quiet stars, contributions to the transmission signal from active stellar surfaces can produce ~1% changes in the line core. It is therefore critical that these contrast signals be differentiated from true absorption features in the planetary atmosphere. Here we present our work on simulating the contrast effect for an active stellar surface. We discuss the particular case of HD 189733 b, a well-studied hot Jupiter orbiting an active K-dwarf, due to the plethora of atomic absorption signals reported in its atmosphere.Specifically, we focus on Hα to address recent suggestions that the measured in-transit signals are a result of stellar activity. In the contrast model we include center-to-limb variations and calculate limb darkening parameters as a function of wavelength across the line of interest. The model includes contributions to the spectrum from spots, faculae and plages, filaments, and the bare stellar photosphere. Stellar rotation is also included. We find that it is very difficult to reproduce the measured in-transit Hα signals for reasonable active region parameters. In addition, it is difficult to create an in-transit contrast signature that lasts for the duration of the transit unless the planet is crossing an active latitudinal belt and is always obscuring active regions. This suggests that the Hα measurements arise predominantly in the planetary atmosphere. However, the contrast effect likely contributes to these signals. Furthermore, our results could be

  3. 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

    introduire un parametre d'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)

  4. 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

  5. Transitioning GONG data processing to NOAA SWPC operations

    Science.gov (United States)

    Reinard, A.; Marble, A.; Hill, F.; Berger, T. E.

    2015-12-01

    The NOAA Space Weather Prediction Center (SWPC) is the nation's official source of space weather watches, warnings, and alerts, providing 24x7 forecasting and support to critical infrastructure operators around the world. Observations of the conditions on the Sun are crucial for determining when and if a warning is needed. The Global Oscillation Network Group (GONG) operated by the National Solar Observatory (NSO) consists of six ground stations, allowing continuous observations of the Sun. Of particular interest for space weather purposes are the H-alpha images and magnetograms. The H-alpha data are used to identify filaments and their eruptions, to assess active region evolution and plage extent, and to help localize flare locations. The magnetograms are used to identify neutral lines, to examine potential shearing areas and to characterize the magnetic structure of active regions. GONG magnetograms also provide the initial condition for models of solar wind expansion through the heliosphere such as the WSA-Enlil model. Although beyond the scope of current space weather applications, GONG helioseismology products can be used to assess active region emergence on the far side of the Sun and to indicate the flaring potential of a front-side active region. These products are being examined as future tools in flare prediction. NSO has operated GONG as a science facility since 1995 and has provided processed space weather data products to NOAA via public internet connections for the past several years. In 2014 the White House Office of Management and Budget (OMB) requested that NOAA transition the GONG network to an operational space weather asset in order to ensure the continued flow of critical magnetogram data for solar wind models. NSO will continue to operate and manage the instruments and sites, but the H-alpha images and 10 minute averaged magnetogram data will be sent directly to SWPC for processing and use in space weather modeling. SWPC will make these data

  6. Transition de phase quantique de type verrouillage-deverrouillage dans les canaux lineaires coherents des phases en rayures dans les doubles puits quantiques sous champ magnetique perpendiculaire

    Science.gov (United States)

    Faribault, Alexandre

    On peut creer un gaz electronique bidimensionnel en utilisant le potentiel de confinement d'une couche mince d'un semiconducteur dans un substrat fait d'une autre semiconducteur de gap plus eleve. L'ajout d'un champ magnetique perpendiculaire au plan de confinement modifie de facon drastique les proprietes du gaz electronique. Pour des densites et des valeurs du champ magnetique adequatement choisies, on obtient un etat fondamental en onde de densite de charge. Dans un systeme compose de deux de ces gaz bidimensionnels suffisamment rapproches l'un de l'autre, on prevoit theoriquement l'existence d'un etat fondamental compose d'une onde de densite de charge dans chacun des puits et d'une serie de regions lineaires ou l'on a une delocalisation coherente des electrons entre les deux puits. Dans cette these, on etudie le comportement a temperature nulle de cet etat fondamental en rayures coherentes. L'etude numerique des modes collectifs de ces phases laisse croire qu'un deverrouillage des canaux coherents est envisageable dans ce systeme. Afin d'etudier cette possibilite, nous construisons d'abord un modele effectif de canaux quasi-unidimensionnels couples qui permettent de reproduire correctement les excitations collectives a basse energie de la phase en rayures coherentes du double puits quantique. Dans un systeme de coordonnees adequatement choisi, ces excitations peuvent etre decrites par des ondes de pseudospin. Les parametres de ce modele effectif simple peuvent etre extraits des calculs des fonctions de reponse realises dans l'approximation Hartree-Fock dependante du temps (appelee aussi Generalized Random Phase Approximation). On constate l'efficacite de ce modele a decrire la dynamique basse energie du systeme pour une certaine plage de distances inter-puits. En retirant de ce modele les contributions a l'hamiltonien provenant des couplages de type Josephson entre les canaux, on obtient alors un systeme ou les canaux sont deverrouilles. Un traitement en

  7. The GAPS programme with HARPS-N at TNG. VII. Putting exoplanets in the stellar context: magnetic activity and asteroseismology of τ Bootis A

    Science.gov (United States)

    Borsa, F.; Scandariato, G.; Rainer, M.; Bignamini, A.; Maggio, A.; Poretti, E.; Lanza, A. F.; Di Mauro, M. P.; Benatti, S.; Biazzo, K.; Bonomo, A. S.; Damasso, M.; Esposito, M.; Gratton, R.; Affer, L.; Barbieri, M.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Covino, E.; Desidera, S.; Fiorenzano, A. F. M.; Gandolfi, D.; Harutyunyan, A.; Maldonado, J.; Micela, G.; Molaro, P.; Molinari, E.; Pagano, I.; Pillitteri, I.; Piotto, G.; Shkolnik, E.; Silvotti, R.; Smareglia, R.; Southworth, J.; Sozzetti, A.; Stelzer, B.

    2015-06-01

    Aims: We observed the τ Boo system with the HARPS-N spectrograph to test a new observational strategy aimed at jointly studying asteroseismology, the planetary orbit, and star-planet magnetic interaction. Methods: We collected high-cadence observations on 11 nearly consecutive nights and for each night averaged the raw FITS files using a dedicated software. In this way we obtained spectra with a high signal-to-noise ratio, used to study the variation of the Ca ii H&K lines and to have radial velocity values free from stellar oscillations, without losing the oscillations information. We developed a dedicated software to build a new custom mask that we used to refine the radial velocity determination with the HARPS-N pipeline and perform the spectroscopic analysis. Results: We updated the planetary ephemeris and showed the acceleration caused by the stellar binary companion. Our results on the stellar activity variation suggest the presence of a high-latitude plage during the time span of our observations. The correlation between the chromospheric activity and the planetary orbital phase remains unclear. Solar-like oscillations are detected in the radial velocity time series: we estimated asteroseismic quantities and found that they agree well with theoretical predictions. Our stellar model yields an age of 0.9 ± 0.5 Gyr for τ Boo and further constrains the value of the stellar mass to 1.38 ± 0.05 M⊙. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF at the Spanish Observatorio Roque de los Muchachos of the IAC in the frame of the program Global Architecture of the Planetary Systems (GAPS).Full Table 1 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/578/A64

  8. 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

  9. 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

  10. 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

  11. 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:

  12. 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

  13. Mid-trimester maternal serum AFP and hCG as markers of preterm and term adverse pregnancy outcomes.

    Science.gov (United States)

    Tancrède, Sabrina; Bujold, Emmanuel; Giguère, Yves; Renald, Marie-Hélène; Girouard, Joel; Forest, Jean-Claude

    2015-02-01

    risque d’IGIMP à terme. Lorsque la croissance fœtale se situe dans la plage normale, les femmes qui présentent des taux sériques élevés d’AFP ou de hCG devraient recevoir des soins de grossesse standard, une fois qu’elles ont atteint 37 semaines de gestation.

  14. 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

  15. Geoconservation and geodiversity for sustainable development in Madagascar

    Directory of Open Access Journals (Sweden)

    Tsilavo Raharimahefa

    2012-12-01

    conservation de la diversité géologique ou géodiversité, qui s’applique généralement à un endroit spécifique désigné en tant que géosite, dans lequel on reconnait des éléments et des dispositifs géologiques importants qui méritent d’être protégés, préservés et gérés comme par exemple dans les domaines de la paléontologie, la géomorphologie, l’hydrologie et la pédologie. La géodiversité de Madagascar compte parmi les plus spectaculaires au monde, allant des rares gisements de minéraux à des paysages et des reliefs spectaculaires, en passant par de belles plages et des grottes qui sont autant de richesses qui pourraient être classées en tant que patrimoine géologique mondial. Face à la dégradation rapide de la géodiversité à Madagascar, il est urgent d’adopter une politique efficace de géoconservation de nombreux sites au profit de la population locale, qui devra aussi permettre de donner un coup de pouce au progrès vers le développement durable du pays.

  16. 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

    enrichi en isotope U{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)

  17. 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).

  18. 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.

  19. 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

  20. Conservative Management of Cervical Ectopic Pregnancy.

    Science.gov (United States)

    Murji, Ally; Garbedian, Kimberley; Thomas, Jacqueline; Cruickshank, Barbara

    2015-11-01

    Objectif : Évaluer l’innocuité et l’efficacité de la prise en charge conservatrice des grossesses ectopiques cervicales. Méthodes : Nous avons mené une analyse rétrospective de tous les cas de grossesse ectopique cervicale diagnostiqués au sein de notre centre universitaire tertiaire entre janvier 2002 et juillet 2014. Le diagnostic de grossesse ectopique cervicale a été établi par échographie transvaginale, conformément aux critères publiés. Les décisions quant à la prise en charge ont été prises par les cliniciens concernés. Résultats : Une grossesse ectopique cervicale a été diagnostiquée chez 27 femmes (âge médian : 34 ans). Les deux tiers d’entre elles étaient nullipares et 44 % (12/27) ont signalé une infertilité. L’âge gestationnel moyen au moment du diagnostic était de sept semaines. Le taux sérique médian de gonadotrophine chorionique humaine était de 11 300 UI/l (plage : de 610 à 163 700). Une activité cardiaque fœtale était présente dans 19 grossesses (70 %). Les saignements vaginaux constituaient la présentation la plus courante; de tels saignements étaient présents dans 23 cas (85 %). Trois femmes ont connu une hémorragie aiguë constituant un danger de mort. Tous les cas ont fait l’objet d’une prise en charge conservatrice réussie qui a permis la préservation de l’utérus. Le méthotrexate administré par voie générale (protocole à dose unique ou à doses multiples) constituait l’élément principal du traitement. Parmi les autres interventions à effraction minimale, on trouvait l’injection (orientée par échographie) de chlorure de potassium dans la grossesse, l’embolisation des artères utérines, la ligature vaginale des rameaux cervicaux des artères utérines et la dilatation-curetage (avec ou sans infiltration cervicale de vasopressine diluée et tamponnement par sonde de Foley). Conclusion : Le recours à du méthotrexate administré par voie générale, seul

  1. 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.

  2. 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

  3. 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

  4. Microgenerateurs electriques a base d'oscillateurs thermiques

    Science.gov (United States)

    Leveille, Etienne

    Dans un contexte de developpement durable et d'automatisation de notre environnement, l'utilisation de capteurs sans-fil distribues est croissante. Hors l'usage et le remplacement de piles s'avere couteux. La consommation energetique de plus en plus faible de l'electronique rend l'extraction energetique de l'energie ambiante envisageable. La chaleur residuelle est une source d'energie interessante puisqu'elle est la forme finale de la majeure partie de l'energie utilisee par l'humain. Cependant, a petite echelle, seuls les elements thermoelectriques sont disponibles. Les presents travaux s'interessent donc a explorer et comparer des mecanismes de generation alternatifs. Puisque la majorite des mecanismes de transduction alternatifs sont dynamiques, leur utilisation requiert une transformation de l'energie thermique continue en oscillations. Les mecanismes etudies ont donc tous en commun de posseder un oscillateur thermique en plus d'un mecanisme de transduction vers la forme d'energie electrique. Parmi les divers mecanismes identifies, deux sont etudies en details pour comprendre leurs comportements ainsi que connaitre leur efficacite et leur puissance potentielle. Le premier generateur etudie theoriquement est base sur le changement de ferromagnetisme d'une masse suspendue par des ressorts au-dessus d'un aimant. Les comportements du modele developpe correspondent aux comportements reportes dans la litterature. Deux parametres de conception principaux ont ete identifies, permettant un controle de la frequence, de la plage de temperatures d'operation. De plus le mecanisme peut operer avec de faibles differences de temperature et des temperatures proches de l'ambiant, ouvrant la porte a des applications utilisant la chaleur du corps humain. L'utilisation de materiau pyroelectrique comme mecanisme de transduction pourrait offrir des densites de puissance electrique envisageables de l'ordre de 1mW/cm3. Le second generateur etudie experimentalement est base sur l

  5. 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.

  6. 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.

  7. Condicionantes del turismo sustentable en el caribe mexicano Conditions of sustainable tourism on the Caribbean coast of Mexico Les conditions du tourisme soutenable sur la côté caribéenne du Mexique.

    Directory of Open Access Journals (Sweden)

    Rosalía Gómez Uzeta

    2011-09-01

    Full Text Available La concurrence internationale sur le marché touristique a des effets négative sur le comportement des flux touristiques américains sur les rivages caribéens du Mexique. La massification des flux a mis en évidence les limites du modèle traditionnel basé sur l'offre « soleil et plage  » commune à l’ensemble de l’espace carïbéen. Pour cette raison, il est nécessaire de repenser de nouvelles façons de soutenir le développement du tourisme, de la décentralisation des fonctions politiques et administratives des trois paliers de gouvernement, et de chercher à renforcer les synergies régionales pour renforcer les possibilités de diversification du développement autour de nouvelles attractions et offres provenant des marchés locaux.Cette stratégie permettra de promouvoir la durabilité de l'économie régionale et d'État et de consolider un projet de développement viable à long terme.The competition on the international tourism market has negative effects on the behavior of American’ tourist flows on the Caribbean coast of Mexico. The mass flows has highlighted the limitations of traditional model based on the offer "sun and beach" common throughout the Caribbean area. For this reason, we need to rethink new ways to support development tourism, the decentralization of political and administrative functions of the three levels of government, and seek to strengthen regional synergies to enhance diversification opportunities around the development of new attractions and offers from local markets.This strategy will promote the sustainability of the regional economy and state and consolidate a sustainable development project in the long term.Existen condiciones de competencia internacional que han afectado negativamente el comportamiento del flujo turístico norteamericano al Caribe Mexicano, ello ha puesto en evidencia la vulnerabilidad del modelo tradicional basado en la oferta de “sol y playa”, que se ha agrava en la

  8. Magnesium sulphate for the management of preeclampsia and eclampsia in low and middle income countries: a systematic review of tested dosing regimens.

    Science.gov (United States)

    Gordon, Rebecca; Magee, Laura A; Payne, Beth; Firoz, Tabassum; Sawchuck, Diane; Tu, Domena; Vidler, Marianne; de Silva, Dane; von Dadelszen, Peter

    2014-02-01

    Objectif : Procéder à une analyse systématique des schémas posologiques de sulfate de magnésium (MgSO4) mis à l’essai dans des pays à revenu faible ou intermédiaire (PRFI) chez des femmes présentant une prééclampsie (prévention) et/ou une éclampsie (traitement). Sources de données : Nous avons mené des recherches dans les bases de données Medline, EMBASE, IPA, CINAHL, CDSR et CENTRAL afin d’en tirer les publications anglophones pertinentes. Sélection des études : Notre recherche nous a menés à 753 publications, dont 26 (10 essais comparatifs randomisés et 16 études observationnelles) ont évalué l’utilisation de MgSO4 dans des cas de prééclampsie et/ou d’éclampsie au sein de PRFI identifiés par la Banque mondiale. Extraction de données : Indépendante, menée par deux auteurs. Synthèse des données : Vingt-cinq études ont été menées en milieu hospitalier et une étude l’a été en milieu communautaire. Les taux d’éclampsie étaient habituellement inférieurs à 5 % (médiane : 3,0 %, plage : 0,0 % - 26,5 %) même lorsque du MgSO4 était administré pour contrer l’éclampsie. Lorsque les posologies utilisées s’éloignaient des posologies standard Pritchard ou Zuspan, pratiquement chacune d’entre elles (n = 22) réduisait la dose de MgSO4 ou la durée du traitement, la raison la plus couramment citée étant la présence de préoccupations au sujet de la sûreté maternelle, des coûts ou de la disponibilité des ressources. Quatre essais ayant comparé le seul recours à une dose de mise en charge (4 g IV + 10 g IM) au recours à une dose de mise en charge et à une dose d’entretien de 5 g/4 h IM n’ont constaté aucune différence en matière de récurrence de l’éclampsie (RR, 1,64; IC à 95 %, 0,48 - 5,65, n = 396). Une étude a constaté une récurrence moindre de l’éclampsie associée à l’administration d’une dose de mise en charge de MgSO4 en milieu communautaire avant l

  9. Cardiovascular responses to millet pounding activity among women in a rural community in Northeastern Nigeria.

    Science.gov (United States)

    Oyeyemi, Adetoyeje Y; Jajimaji, Fati; Oyeyemi, Adewale L; Jabbo, Abdul-Hameed A

    2017-01-01

    la dépense énergétique au cours de cette activité et si l'activité peut être considérée comme une activité légère, modérée ou vigoureuse Intensité est inconnue. Objectif: La présente étude visait à mieux comprendre les dépenses énergétiques au cours de la Les réponses cardiovasculaires à l'activité battue du mil, et d'explorer les différences possibles dans la réponse entre les femmes qui pound millet comme leur (Millet pounders habituels) et ceux qui pound millet seulement pour leur propre cuisine à la maison, mais pas comme un emploi (pounders nonhabituel). Méthodes: Un total de quarante femmes apparemment saines ont effectué une activité de pilage du mil en position debout pendant 15 min de durée, et leurs Les paramètres cardiovasculaires, y compris la fréquence cardiaque (FC), la pression artérielle systolique (PAS) et les pressions artérielles diastoliques (PAD) (RPE) au repos, et immédiatement après l'activité de pilonnage ont été évalués. Résultats: Augmentation significative des taux de On a observé des paramètres situés dans la plage des valeurs de 7-12, 1-5 et 19-21 points au-dessus des niveaux de repos pour la PAS, la PAD et la HR respectivement. On a également observé une PAS significativement plus élevée pour les pounders habituels que pour les pounders non habituels, alors que la PPE était Significativement plus élevé pour les pounders non habituels que pour les pounders habituels en réponse à pounding. Cette étude suggère Que le broyage du millet souligne sensiblement suffisamment le système cardiovasculaire pour placer l'activité dans la catégorie d'intensité modérée. D'autres études sur le coût de l'énergie de cette corvée maison, en utilisant une instrumentation qui est capable de mesure directe de la consommation d'oxygène, est justifiée.

  10. 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

  11. 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

  12. 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

  13. TDC Offset Estimation from Motored Cylinder Pressure Data based on Heat Release Shaping Estimation du décalage de PMH à partir de données de pression de cylindre moteur basées sur la conformation de libération de chaleur

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    Tunestål P.

    2011-10-01

    éthode proposée utilise une optimisation des moindres carrés non linéaire pour déterminer la combinaison de rapport de chaleur spécifique et de décalage de PMH qui rend la puissance de perte de chaleur aussi constante que possible. Un sous-problème important consiste à déterminer la localisation de pression de pic avec une haute précision. L’application d’une série de Fourier du troisième ordre à la pression de cylindre moteur permet l’estimation du maximum de pression moyennant un écart-type de 0,005° d’angle de bras de manivelle (AM et elle peut être également utilisée à la place de la pression mesurée afin de réduire l’incertitude de l’estimation du PMH d’environ 50 %. L’écart-type d’une estimation de PMH de cycle unique est approximativement de 0,025° d’AM lors de l’utilisation d’une résolution de bras de manivelle de 0,2° d’AM pour les mesures. L’erreur systématique de l’estimation de PMH se situe dans la plage allant de 0 à 0,02° d’AM par comparaison à la fois avec les mesures réalisées au moyen d’un détecteur de PMH et avec des cycles moteur simulés. La méthode peut être utilisée à la fois à des fins d’étalonnage et de diagnostics à bord, par exemple pendant un démarrage, une coupure de carburant ou un arrêt du moteur. La série de Fourier du troisième ordre appliquée s’accompagne d’une pénalisation de calcul significative mais, puisqu’elle n’est appliquée que de façon très intermittente, ceci ne doit pas poser un problème sérieux.

  14. Une alternative au cobalt pour la synthese de nanotubes de carbone monoparoi par plasma inductif thermique

    Science.gov (United States)

    Carrier, Jean-Francois

    Les nanotubes de carbone de type monoparoi (C-SWNT) sont une classe recente de nanomateriaux qui ont fait leur apparition en 1991. L'interet qu'on leur accorde provient des nombreuses proprietes d'avant-plan qu'ils possedent. Leur resistance mecanique serait des plus rigide, tout comme ils peuvent conduire l'electricite et la chaleur d'une maniere inegalee. Non moins, les C-SWNT promettent de devenir une nouvelle classe de plateforme moleculaire, en servant de site d'attache pour des groupements reactifs. Les promesses de ce type particulier de nanomateriau sont nombreuses, la question aujourd'hui est de comment les realiser. La technologie de synthese par plasma inductif thermique se situe avantageusement pour la qualite de ses produits, sa productivite et les faibles couts d'operation. Par contre, des recherches recentes ont permis de mettre en lumiere des risques d'expositions reliees a l'utilisation du cobalt, comme catalyseur de synthese; son elimination ou bien son remplacement est devenu une preoccupation importante. Quatre recettes alternatives ont ete mises a l'essai afin de trouver une alternative plus securitaire a la recette de base; un melange catalytique ternaire, compose de nickel, de cobalt et d'oxyde d'yttrium. La premiere consiste essentiellement a remplacer la proportion massique de cobalt par du nickel, qui etait deja present dans la recette de base. Les trois options suivantes contiennent de nouveaux catalyseurs, en remplacement au Co, qui sont apparus dans plusieurs recherches scientifiques au courant des dernieres annees: le dioxyde de zircone (ZrO2), dioxyde de manganese (MnO2) et le molybdene (Mo). La methode utilisee consiste a vaporiser la matiere premiere, sous forme solide, dans un reacteur plasma a haute frequence (3 MHz) a paroi refroidi. Apres le passage dans le plasma, le systeme traverse une section dite de "croissance", isolee thermiquement a l'aide de graphite, afin de maintenir une certaine plage de temperature favorable a la

  15. Use of glycated hemoglobin and waist circumference for diabetic screening in women with a history of gestational diabetes.

    Science.gov (United States)

    Gingras, Véronique; Tchernof, André; Weisnagel, S John; Robitaille, Julie

    2013-09-01

    Objectif : Bien que leur risque de présenter un diabète de type 2 connaisse une hausse considérable, les femmes ayant déjà connu un diabète sucré gestationnel (DSG) ne bénéficient pas de services de dépistage adéquats à la suite de leur grossesse. L’identification d’une méthode de dépistage moins lourde pourrait accroître les taux de dépistage postpartum. Nous avions pour objectif d’examiner le caractère adéquat des mesures du taux d’hémoglobine glyquée (A1C) et du tour de taille (TT) pour ce qui est de la détection de l’altération du métabolisme du glucose chez les femmes ayant déjà connu un DSG. Méthodes : L’analyse portait sur 178 femmes ayant connu un DSG entre 2003 et 2010. Le TT et le taux d’A1C ont été mesurés, et une épreuve d’hyperglycémie provoquée par voie orale (75 g, 2 h) a été menée. Le prédiabète a été défini comme étant une glycémie à jeun (GJ) ≥ 5,6 et < 7,0 mmol/l ou une glycémie à 2 heures (G-2 h) ≥ 7,8 et < 11,0 mmol/l, tandis que le diabète de type 2 a été défini comme étant une GJ ≥ 7,0 mmol/l et/ou une G-2 h ≥ 11,1 mmol/l. Des analyses de sensibilité et de spécificité ont été menées. Résultats : L’âge moyen des sujets était de 36,4 ± 4,8 ans et le dépistage s’est déroulé, en moyenne, 3,5 ± 1,9 ans à la suite de l’accouchement. La combinaison d’un taux de A1C ≥ 5,7 % et d’un TT ≥ 88 cm pour détecter le prédiabète comptait une sensibilité de 76 % et une spécificité de 62 %; pour ce qui est de la détection du diabète de type 2, cette combinaison comptait une sensibilité de 91 % et une spécificité de 34 %. Par comparaison avec les femmes qui présentaient un taux d’A1C et un TT se situant dans la plage normale, les femmes qui présentaient un taux d’A1C ≥ 5,7 % et un TT ≥ 88 cm étaient plus susceptibles de connaître un diabète de type 2 (RC, 4,4; IC à 95 %, 2,0 - 9,9). Conclusion : Ces analyses

  16. Progress in the Measurement and Study of Solar Irradiance%太阳辐照的观测研究进展

    Institute of Scientific and Technical Information of China (English)

    徐景晨; 李可军

    2011-01-01

    radiometers started in 1978, and it was consequently know as the “solar constant”. But now we know that besides modulated by the 11-year solar cycle, it varies at all time scales at which it has been measured, i.e., minutes to decades, and most probably, on longer time scales as well.The variability of solar irradiance has important implication for our understanding of solar internal structure, solar activities, global changes in the Earth's climate system, and the solarterrestrial relationship. Thus, accompanied with more and more data from space-borne satellites during the recent three decades, lots of work has been done. It is believed that Irradiance variability on timescales from minutes to hours is mainly caused by convection. Short-term changes of total solar irradiance on timescales of few days to weeks are dominated by magnetic structures.Over the solar cycle, variations of 0.1% is believed to come mainly from the combination of the sunspots blocking and the intensification due to bright faculae, plages, and network elements.Some indexes seems to have certain relationship with the variations of solar irradiance, for example sunspot number, Mg Ⅱ index, faculae area, F10.7 flux index, solar modulation of cosmogenic isotopes such as 14C and 10B and other solar related records. Based on this knowledge as well as the measurements of solar surface magnetic field, some models have been developed to reconstruct both total and spectral solar irradiance. Some of them are very successful and can account for most of the variance in the observed irradiance time series. There are still some problems with the three commonly used composite data, because significant uncertainties remain related to the calibration of the instruments and their degradation over time, and this uncertainty is a serious problem underlying current solar-climate research.In Sect. 2 the total and spectral solar irradiance measurements are reviewed. Sect. 3 describes a statistical analysis of one of

  17. 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

  18. Prenatal Diagnosis Procedures and Techniques to Obtain a Diagnostic Fetal Specimen or Tissue: Maternal and Fetal Risks and Benefits.

    Science.gov (United States)

    Wilson, R Douglas; Gagnon, Alain; Audibert, François; Campagnolo, Carla; Carroll, June; Brock, Jo-Ann; Chong, Karen; Johnson, Jo-Ann; MacDonald, William; Okun, Nanette; Pastuck, Melanie; Vallee-Pouliot, Karine

    2015-07-01

    offrir, aux femmes enceintes exposées à des risques, des services de counseling au sujet des différents niveaux du dépistage génétique fœtal, de façon à ce qu’elles puissent bien comprendre le niveau du dépistage qui leur est offert et les types de résultats auxquels elles sont en droit de s’attendre. (III-B) 2. Les fournisseurs de soins de santé devraient offrir, aux femmes enceintes exposées à des risques, des services de counseling au sujet de la ou des techniques de diagnostic génétique in utero qui sont associées aux options de dépistage génétique fœtal et en passer en revue les risques et les avantages dans le cadre du processus de consentement éclairé. (III-A) 3. Dans le cadre des services de counseling sur les risques et les avantages, les fournisseurs de soins de santé devraient aviser leurs patientes des meilleures estimations suivantes en ce qui concerne le taux de fausse couche : a. amniocentèse = 0,5%-1,0 % (plage : 0,17-1,53 %) (I) b. prélèvement de villosités choriales = 0,5 %-1,0 % (I) et c. cordocentèse (ou prélèvement percutané de sang ombilical) = 1,3 %, dans le cas des fœtus sans anomalies, et 1,3 %-25 %, dans le cas des fœtus présentant une ou des anomalies ou un retard de croissance intra-utérin. (II-2A).

  19. L’océan au coeur de la Grande Île : Les aires marines protégées, un outil de développement durable pour Madagascar

    Directory of Open Access Journals (Sweden)

    Rémi A. Ratsimbazafy

    2011-06-01

    Full Text Available Grande Île de l’océan Indien, Madagascar apparaît comme une véritable « île continent » avec une superficie de plus de 590 000 km² et plus de 5000 km de côtes. Ses zones marines et côtières abritent une variété d’écosystèmes et d’habitats parmi lesquels les récifs coralliens, mangroves, dunes, lagons, plages sableuses, herbiers de phanérogames, estuaires, îles et îlots auxquels sont associés de nombreuses espèces de coraux, poissons, reptiles, crustacés, mollusques, échinodermes. Les écosystèmes les plus connus sont certainement les récifs coralliens avec une superficie de près de 5000 km² et les mangroves qui s’étendent sur plus de 3000 km² principalement sur les rivages occidentaux de l’île. Ils apportent d’énormes bénéfices socio-économiques aux communautés locales grâce à la pêche et aux activités touristiques sans oublier les services écologiques que ces écosystèmes assurent pour l’équilibre de la planète et le bien-être de l’Homme. Au vu de l’importance de ces zones marines et côtières et dans le but de les préserver face aux menaces et pressions d’origine anthropique et naturelle, Madagascar s’est résolument investie dans la création et la mise en place d’aires marines protégées et de réserves marines afin de contribuer au bien-être des communautés locales qui en dépendent. Dans cette optique, le Système d’Aires Protégées de Madagascar, SAPM, a été mis en place pour offrir les outils appropriés de gestion, de gouvernance et de planification dans l’objectif de tripler la surface des aires protégées, ce qui la porterait de 1,7 à près de 6 millions d’hectares (Vision Durban. La première aire marine protégée a été officiellement créée en 1989 avec le parc marin de Nosy Antafana intégré à la Réserve de Biosphère de Mananara Nord, suivie par les trois parcelles marines du Parc National de Masoala. Vingt ans après le premier parc marin

  20. Climatic influence on slope dynamics and shoreline variations: examples from Marche region (Central Italy

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    Domenico Aringoli

    2007-12-01

    ècles, peut être attribuée à l'aggravation du climat pendant cette période.Dans la bande côtière c'est dans l'embouchure fleuve Chienti qu'est analysée l'évolution morphodynamique. Ce delta est constitué en majorité de graviers calcaires et marno-calcaires. Ce cours d'eau, long de 91 km, prend sa source sur le versant septentrional des Monts Sibyllins et a un bassin hydrographique, de 1250 km2. Il est un des principaux cours d'eau des Marches et il coupe perpendiculairement les principales unités structurales de l'Apennin d'Ombrie-Marches. À partir des sources historiques, on a pu établir que la ligne de rivage a connu, près de l'embouchure, une avancée relativement forte jusqu'à la fin du XVIIIème siècle. Cette avancée se renforce entre 1810 et 1935 (3,2 m/an. En revanche, depuis 1935, on observe un recul du delta (3,5 m/an. Dans la zone urbaine de Porto Civitanova, située au nord de l'embouchure, une étude détaillée de la ligne de rivage durant les trois derniers siècles, montre une avancée moyenne pendant la période 1705-1935 (environ 1,1 m/an suivie d'une forte accélération à partir de 1935 (2,8 m/an. Cette accélération peut être liée à la présence d'ouvrages portuaires, commencés en 1932 et achevés en 1938. Dans l'interprétation complexe des processus responsables de l'évolution de l'embouchure du Chienti, comme dans celle d'autres cours d'eau des Marches, il est tenu compte non seulement du facteur anthropique, déjà signalé plusieurs fois par les auteurs, mais aussi de l'action retardée dans le temps des conditions climatiques froides et humides post-médiévales. En effet, la forte avancée de la plage entre 1810 et 1935 trouve son explication dans l'arrivée à l'embouchure de quantités considérables de matériaux dont la texture favorise les processus de sédimentation (graviers. Leur provenance est la conséquence de l'érosion des dépôts détritiques de la zone des montagnes et des hautes collines par l

  1. Intrauterine growth restriction: screening, diagnosis, and management.

    Science.gov (United States)

    Lausman, Andrea; Kingdom, John; Gagnon, Robert; Basso, Melanie; Bos, Hayley; Crane, Joan; Davies, Gregory; Delisle, Marie-France; Hudon, Lynda; Menticoglou, Savas; Mundle, William; Ouellet, Annie; Pressey, Tracy; Pylypjuk, Christy; Roggensack, Anne; Sanderson, Frank

    2013-08-01

    organismes connexes, dans des collections de directives cliniques, dans des registres d’essais cliniques et auprès de sociétés de spécialité médicale nationales et internationales. Valeurs : La qualité des résultats est évaluée au moyen des critères décrits dans le rapport du Groupe d’étude canadien sur les soins de santé préventifs (Tableau). Avantages, désavantages et coûts : La mise en œuvre des recommandations formulées aux présentes devraient accroître la reconnaissance du RCIU par les cliniciens et guider l’intervention, dans les cas où cela s’avère approprié. La mise en œuvre d’un suivi optimal à long terme des nouveau-nés présentant un diagnostic de RCIU pourrait améliorer leur santé à long terme. Déclarations sommaires 1. Dans le cas d’un fœtus in utero, l’hypotrophie fœtale se définit comme suit : un poids fœtal estimé inférieur au 10e percentile au moment de l’échographie. Ce diagnostic n’indique pas nécessairement la présence d’anomalies de croissance pathologiques et pourrait simplement décrire un fœtus se situant dans la partie inférieure de la plage normale. (III) 2. Par « retard de croissance intra-utérin », on entend un fœtus présentant un poids fœtal estimé inférieur au 10e percentile au moment de l’échographie qui, en raison d’un processus pathologique, n’a pas atteint son potentiel de croissance biologiquement déterminé (III). L’estimation clinique du poids fœtal ou de la hauteur utérine compte une sensibilité et une spécificité faibles, et ne devrait pas être utilisée dans le cadre du diagnostic du retard de croissance intra-utérin. La présence de ce dernier devrait être prise en considération aux fins du diagnostic différentiel lorsque l’on constate que le fœtus présente une hypotrophie fœtale. (II-I) 3. Le dépistage efficace du retard de croissance intra-utérin nécessite une datation précise et comprend une analyse des antécédents menstruels de la m

  2. 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