Groupe de Recherche en Astronomie et Astrophysique du Languedoc, UMR 5024,
Université Montpellier II,
Place Eugène Bataillon,
2 Département de Physique, Université de Montréal, Montréal, PQ, H3C 3J7, Canada
3 Laboratoire Universitaire d’Astrophysique de Nice, UMR 6525, Université de Nice – Sophia Antipolis, Parc Valrose, 06108 Nice Cedex 2, France
4 Institut für Astronomie, Universität Wien, Türkenschanzstrasse 17, 1180 Wien, Austria
5 Department of Physics and Astronomy, Open University, Walton Hall, Milton Keynes MK7 6AA, UK
Received: 9 September 2009
Accepted: 17 June 2010
Aims. Abundances of 15 chemical elements have been derived for 28 F and 16 A stars members of the Hyades open cluster in order to set constraints on self-consistent evolutionary models that include radiative and turbulent diffusion.
Methods. A spectral synthesis, iterative procedure was applied to derive the abundances from selected high-quality lines in high-resolution, high-signal-to-noise spectra obtained with SOPHIE and AURELIE at the Observatoire de Haute Provence.
Results. The abundance patterns found for A and F stars in the Hyades resemble those observed in Coma Berenices and Pleiades clusters. In graphs representing the abundances versus the effective temperature, A stars often display much more scattered abundances around their mean values than the coolest F stars do. Large star-to-star variations are detected in the Hyades A dwarfs in their abundances of C, Na, Sc, Fe, Ni, Sr, Y, and Zr, which we interpret as evidence of transport processes competing with radiative diffusion. In A and Am stars, the abundances of Cr, Ni, Sr, Y, and Zr are found to be correlated with that of Fe as in the Pleiades and in Coma Berenices. The ratios [C/Fe] and [O/Fe] are found to be anticorrelated with [Fe/H] as in Coma Berenices. All Am stars in the Hyades are deficient in C and O and overabundant in elements heavier than Fe but not all are deficient in Ca and/or Sc. The F stars have solar abundances for almost all elements except for Si. The overall shape of the abundance pattern of the slow rotator HD 30210 cannot be entirely reproduced by models including radiative diffusion and different amounts of turbulent diffusion.
Conclusions. While part of the discrepancies between derived and predicted abundances could come from non-LTE effects, including competing processes such as rotational mixing and/or mass loss seems necessary in order to improve the agreement between the observed and predicted abundance patterns.
Key words: stars: abundances / stars: chemically peculiar / stars: rotation / open clusters and associations: individual: Hyades / diffusion
Tables 5 to 8 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/523/A71
© ESO, 2010