EDP Sciences
Free Access
Volume 386, Number 3, May II 2002
Page(s) 1028 - 1038
Section Formation and evolution of planetary systems
DOI https://doi.org/10.1051/0004-6361:20020280

A&A 386, 1028-1038 (2002)
DOI: 10.1051/0004-6361:20020280

Beryllium abundances in stars hosting giant planets

N. C. Santos1, R. J. García López2, 3, G. Israelian2, M. Mayor1, R. Rebolo2, 4, A. García-Gil2, M. R. Pérez de Taoro2 and S. Randich5

1  Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
2  Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
3  Departamento de Astrofísica, Universidad de La Laguna, Av. Astrofísico Francisco Sánchez s/n, 38206 La Laguna, Tenerife, Spain
4  Consejo Superior de Investigaciones Científicas, Spain
5  INAF/Osservatorio Astrofisico di Arcetri, Largo Fermi 5, 50125 Firenze, Italy

(Received 26 October 2001 / Accepted 22 February 2002 )

We have derived beryllium abundances in a wide sample of stars hosting planets, with spectral types in the range F7V-K0V, aimed at studying in detail the effects of the presence of planets on the structure and evolution of the associated stars. Predictions from current models are compared with the derived abundances and suggestions are provided to explain the observed inconsistencies. We show that while still not clear, the results suggest that theoretical models may have to be revised for stars with T</I>eff<5500 K. On the other hand, a comparison between planet host and non-planet host stars shows no clear difference between both populations. Although preliminary, this result favors a "primordial" origin for the metallicity "excess" observed for the planetary host stars. Under this assumption, i.e. that there would be no differences between stars with and without giant planets, the light element depletion pattern of our sample of stars may also be used to further investigate and constraint Li and Be depletion mechanisms.

Key words: stars: abundances -- stars: chemically peculiar -- stars: evolution -- planetary systems

Offprint request: N. C. Santos, Nuno.Santos@obs.unige.ch

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