A&A 404, 715-727 (2003)
DOI: 10.1051/0004-6361:20030543

Chemical abundances of planet-host stars

Results for alpha and Fe-group elements

A. Bodaghee¹, N. C. Santos^{1, 2}, G. Israelian³ and M. Mayor<sup>1

1</sup>  Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland
²  Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal
³  Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain

(Received 3 February 2003 / Accepted 7 April 2003)

Abstract
In this paper, we present a study of the abundances of Si, Ca, Sc, Ti, V, Cr, Mn, Co, and Ni in a large set of stars known to harbor giant planets, as well as in a comparison sample of stars not known to have any planetary-mass companions. We have checked for possible chemical differences between planet hosts and field stars without known planets. Our results show that overall, and for a given value of [Fe/H], the abundance trends for the planet hosts are nearly indistinguishable from those of the field stars. In general, the trends show no discontinuities, and the abundance distributions of stars with giant planets are high [Fe/H] extensions to the curves traced by the field dwarfs without planets. The only elements that might present slight differences between the two groups of stars are V, Mn, and to a lesser extent Ti and Co. We also use the available data to describe galactic chemical evolution trends for the elements studied. When comparing the results with former studies, a few differences emerge for the high [Fe/H] tail of the distribution, a region that is sampled with unprecedented detail in our analysis.

Key words: stars: abundances -- stars: fundamental parameters -- stars: chemically peculiar -- stars: evolution -- planetary systems -- solar neighborhood

Offprint request: N. C. Santos, Nuno.Santos@oal.ul.pt

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© ESO 2003

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