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Abundances of stars in lower main sequence (Mishenina+, 2008) - VizieR On-line Data Catalog: J/A+A/489/923. Originally published in: 2008A&A...489..923M

hal.structure.identifierAstronomical observatory of Odessa National University [Odessa]
dc.contributor.authorMISHENINA, T. V.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
dc.contributor.authorSOUBIRAN, C.
hal.structure.identifierObservatoire astronomique de Strasbourg [OAS]
dc.contributor.authorBIENAYME, O.
hal.structure.identifierAstronomical observatory of Odessa National University [Odessa]
dc.contributor.authorKOROTIN, S. A.
hal.structure.identifierOdessa Astronomical Observatory
dc.contributor.authorBELIK, S. I.
hal.structure.identifierOdessa Astronomical Observatory
dc.contributor.authorUSENKO, I. A.
hal.structure.identifierAstronomical observatory of Odessa National University [Odessa]
dc.contributor.authorKOVTYUKH, V. V.
dc.date.issued2009
dc.descriptionVizieR On-line Data Catalog
dc.description.abstractEnThe aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars. (3 data files).
dc.language.isoen
dc.subject.enStars: late-type
dc.subject.enAbundances
dc.title.enAbundances of stars in lower main sequence (Mishenina+, 2008) - VizieR On-line Data Catalog: J/A+A/489/923. Originally published in: 2008A&A...489..923M
dc.typeAutre document
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]
bordeaux.page90923
hal.identifierhal-00439388
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00439388v1
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