Volume 425, Number 2, October II 2004
|Page(s)||683 - 695|
|Published online||21 September 2004|
Abundance analysis of targets for the COROT/MONS asteroseismology missions*
II. Abundance analysis of the COROT main targets
Department of Physics and Astronomy, Aarhus University, Bygn. 520, 8000 Aarhus C, Denmark e-mail: firstname.lastname@example.org
2 Department of Astronomy, Kazan State University, Kremlevskaya 18, 420008 Kazan, Russia
3 Observatoire de Paris, LESIA, France
4 Laboratorio de Astrofísica Espacial y Física Fundamental, PO Box 50727, 28080 Madrid, Spain
5 Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, 17, 4000 Liège, Belgium
6 Observatoire de Paris, GEPI, France
7 Institut für Astronomie, Universität Wien, Türkenschanzstrasse 17, 1180 Wien, Austria
8 Laboratoire d'Astrophysique de Marseille, France
9 Laboratoire d'Astrophysique de l'OMP, CNRS UMR 5572, Observatoire Midi-Pyrénées, 14, avenue Edouard Belin, 31400 Toulouse, France
Accepted: 11 June 2004
One of the goals of the ground-based support program for the corot and mons/rømer satellite missions is to characterize suitable target stars for the part of the missions dedicated to asteroseismology. We present the detailed abundance analysis of nine of the potential corot main targets using the semi-automatic software vwa. For two additional corot targets we could not perform the analysis due to the high rotational velocity of these stars. For five stars with low rotational velocity we have also performed abundance analysis by a classical equivalent width method in order to test the reliability of the vwa software. The agreement between the different methods is good. We find that it is necessary to measure abundances extracted from each line relative to the abundances found from a spectrum of the Sun in order to remove systematic errors. We have constrained the global atmospheric parameters Teff, , and [Fe/H] to within K, dex, and 0.1 dex for five stars which are slow rotators (). For most of the stars we find good agreement with the parameters found from line depth ratios, H α lines, Strömgren indices, previous spectroscopic studies, and also determined from the hipparcos parallaxes. For the fast rotators () it is not possible to constrain the atmospheric parameters.
Key words: stars: abundances / stars: fundamental parameters
© ESO, 2004
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