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Your search keyword '"Caroline Soubiran"' showing total 6 results
Start Over Author "Caroline Soubiran" Publisher oxford university press (oup)
6 results on '"Caroline Soubiran"'

1. Chemical composition of stars with massive planets

Author

N. Basak, Vardan Adibekyan, T. V. Mishenina, Caroline Soubiran, V. V. Kovtyukh, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Metallicity, Analytical chemistry, FOS: Physical sciences, chemistry.chemical_element, 01 natural sciences, 7. Clean energy, Planet, Abundance (ecology), 0103 physical sciences, 010303 astronomy & astrophysics, Chemical composition, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, Planetary system, Stars, Astrophysics - Solar and Stellar Astrophysics, chemistry, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Lithium, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract

Stellar parameters of 25 planet-hosting stars and abundances of Li, C, O, Na, Mg, Al, S, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Ni, Zn, Y, Zr, Ba, Ce, Pr, Nd, Sm and Eu, were studied based on homogeneous high resolution spectra and uniform techniques. The iron abundance [Fe/H] and key elements (Li, C, O, Mg, Si) indicative of the planet formation, as well as the dependencies of [El/Fe] on $T_{cond}$, were analyzed. The iron abundances determined in our sample stars with detected massive planets range within -0.3= 0.48 +/-0.07 and =-0.07 +/-0.07, which are slightly lower than solar ones. The Mg/Si ratios range from 0.83 to 0.95 for four stars in our sample and from 1.0 to 1.86 for the remaining 21 stars. Various slopes of [El/Fe] vs. Tcond were found. The dependencies of the planetary mass on metallicity, the lithium abundance, the C/O and Mg/Si ratios, and also on the [El/Fe]-Tcond slopes were considered., Comment: 25 pages, 11 figures, Accepted in MNRAS

Published
2021

2. Observing the metal-poor solar neighbourhood: a comparison of galactic chemical evolution predictions*†

Author

N. Basak, Claudia Travaglio, Benoit Côté, V. V. Kovtyukh, Caroline Soubiran, C. J. Jordan, Brad K. Gibson, S. A. Korotin, Marco Pignatari, Sara Bisterzo, Benjamin Wehmeyer, Friedrich-Karl Thielemann, Adam Paul, C. Ritter, Falk Herwig, T. V. Mishenina, T. I. Gorbaneva, Astronomical observatory of Odessa National University [Odessa], Odessa National I.I.Mechnikov University, M2A 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Unité de recherche Géochimie des Sols et des Eaux (URGSE), Institut National de la Recherche Agronomique (INRA), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Collège de France (CdF (institution))-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA), Helmholtz Centre for Infection Research (HZI), Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Collège de France (CdF)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Institut National de la Recherche Agronomique (INRA), and Institut de Recherche pour le Développement (IRD)-Institut National de la Recherche Agronomique (INRA)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, 010308 nuclear & particles physics, Thermodynamic equilibrium, Neighbourhood (graph theory), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Spectral line, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Metal, Stars, Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), visual_art, 0103 physical sciences, Galaxy formation and evolution, visual_art.visual_art_medium, Dispersion (chemistry), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Atmospheric parameters and chemical compositions for ten stars with metallicities in the region of -2.2< [Fe/H], Comment: 25 pages, 7 figures

Published
2017

3. The non-local thermodynamic equilibrium barium abundance in dwarf stars in the metallicity range of

Author

Caroline Soubiran, S. A. Korotin, T. V. Mishenina, and T. I. Gorbaneva

Subjects
Physics, Opacity, Metallicity, chemistry.chemical_element, Astronomy and Astrophysics, Barium, Astrophysics, 01 natural sciences, Atmosphere, Stars, chemistry, Space and Planetary Science, Abundance (ecology), 0103 physical sciences, Atom, 010306 general physics, 010303 astronomy & astrophysics, Line (formation)
Abstract

We present the results of determination of the barium abundance considering the non-LTE (NLTE) effects in 172 dwarf stars in the metallicity range of -1< [Fe/H]

Published
2011

4. Accurate luminosities for F-G supergiants from Fe ii / Fe i line depth ratios

Author

R. E. Luck, V. V. Kovtyukh, S. I. Belik, M. P. Yasinskaya, F. A. Chekhonadskikh, and Caroline Soubiran

Subjects
Physics, Absolute magnitude, 010504 meteorology & atmospheric sciences, Cepheid variable, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Effective temperature, Stellar classification, 01 natural sciences, Luminosity, Stars, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Supergiant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract

Luminous FG supergiants can be used as extragalactic distance indicators. In order to fully exploit the properties of these bright stars, we must first learn how to measure their luminosities. Based primarily on classical Cepheids and supergiants in clusters and OB associations, we have derived 80 empirical relations connecting the line depth ratios of Fe ii/Fe i lines with the absolute magnitudes Mv and the effective temperatures Teff. These relations have been applied to estimate the absolute magnitudes of 98 FG supergiants with an error of ±0.26 mag. The application range of our calibrations is spectral types F2–G8 and luminosity classes I and II (absolute magnitudes Mv, −0.5 to −8 mag). A comparison of our Mv determinations with values from the literature shows good agreement.

Published
2010

5. Spectroscopic ages and metallicities of stellar populations: validation of full spectrum fitting

Author

Caroline Soubiran, D. Le Borgne, Pierre Ocvirk, Ph. Prugniel, Mina Koleva, University of Sofia, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Sofia University 'St. Kliment Ohridski', Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Astrophysikalisches Institut Potsdam (AIP), Pomies, Marie-Paule, Софийски университет = Sofia University, and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
FOS: Physical sciences, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Blue straggler, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galaxy groups and clusters, 0103 physical sciences, Spectral resolution, Spectroscopy, 010303 astronomy & astrophysics, Physics, Galaxy: stellar content, (Galaxy:) globular clusters: general, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Horizontal branch, Stars, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Globular cluster, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic
Abstract

Fitting whole spectra at intermediate spectral resolution (R = 1000 -- 3000), to derive physical properties of stellar populations, appears as an optimized alternative to methods based on spectrophotometric indices: it uses all the redundant information contained in the signal. This paper addresses the validation of the method and it investigates the quality of the population models together with the reliability of the fitting procedures. We are using two algorithms: STECKMAP, a non-parametric regularized program and NBURSTS a parametric non-linear minimization. We compare three spectral synthesis models for single stellar populations: Pegase-HR, Galaxev (BC03) and Vazdekis/Miles, and we analyse spectra of Galactic clusters whose populations are known from studies of color-magnitude diagrams (CMD) and spectroscopy of individual stars. We find that: (1) The quality of the models critically depends on the stellar library they use. Pegase-HR and Vazdekis/Miles are consistent, while the comparison between Pegase-HR and BC03 shows some systematics reflecting the limitations of the stellar library (STELIB) used to generate the latter models; (2) The two fitting programs are consistent; (3) For globular clusters and M67 spectra, the method restitutes metallicities in agreement with spectroscopy of stars within 0.14 dex; (4) The spectroscopic ages are very sensitive to the presence of a blue horizontal branch (BHB) or of blue stragglers. A BHB morphology results in a young SSP-equivalent age. Fitting a free amount of blue stars in addition to the SSP model to mimic the BHB improves and stabilizes the fit and restores ages in agreement with CMDs studies. This method is potentially able to disentangle age or BHB effects in extragalactic clusters., Comment: accepted in MNRAS; Full version available at http://www-obs.univ-lyon1.fr/labo/perso/prugniel/mina/koleva.pdf

Published
2008

6. The chemical composition ofδScuti★

Author

Alexander V. Yushchenko, V. F. Gopka, Caroline Soubiran, F. A. Musaev, Young-Woon Kang, V. V. Kovtyukh, and Chulhee Kim

Subjects
Physics, Photosphere, Astronomy and Astrophysics, Astrophysics, medicine.disease_cause, Abundance of the chemical elements, Spectral line, Stars, Space and Planetary Science, Abundance (ecology), medicine, Stellar evolution, Chemical composition, Ultraviolet
Abstract

We present chemical abundances in the photosphere of δ Scuti (δ Sct) – a prototype of the class of pulsating variables – determined from the analysis of a spectrum obtained by using the 2-m telescope at the Peak Terskol Observatory and a high-resolution spectrometer with R= 52 000, a signal-to-noise ratio 250 and from International Ultraviolet Explorer spectra. The abundance pattern of δ Sct consists of 49 chemical elements. The abundances of 19 elements have not been investigated previously. The abundances of Pr and Nd obtained from the lines of the second and third spectra are equal. The abundances of heavy elements indicate the overabundances with respect to the solar system values up to 1 dex. The abundance pattern of δ Sct is similar to the abundance patterns of Am–Fm or δ Del type stars. A splitting of the cores of all clean lines is observed for the spectra of δ Sct and HD 57749. This can signify evidence of non-radial pulsations in these stars.

Published
2005

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