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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. Santos1, 2, G. Israelian3 and M. Mayor11 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