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Light elements in stars with exoplanets

Santos, N. C. ; Delgado Mena, E. ; Israelian, G. ; González-Hernández, J. I. ; Gálvez-Ortiz, M. C. ; Mayor, M. ; Udry, S. ; Rebolo, R. ; Sousa, S. ; Randich, S.

In: Proceedings of the International Astronomical Union, 2009, vol. 5, no. S268, p. 291-299

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    Titre
    • Light elements in stars with exoplanets
    Auteur
    • Santos, N. C.. Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal. email: Nuno.Santos@astro.up.pt
    • Delgado Mena, E.. Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain.
    • Israelian, G.. Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain.
    • González-Hernández, J. I.. Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, E-28040, Spain.
    • Gálvez-Ortiz, M. C.. Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB, UK.
    • Mayor, M.. Observatoire de Genève, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland.
    • Udry, S.. Observatoire de Genève, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland.
    • Rebolo, R.. Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain.
    • Sousa, S.. Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal. email: Nuno.Santos@astro.up.pt
    • Randich, S.. INAF/Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Firenze, Italia.
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Proceedings of the International Astronomical Union, 2009, vol. 5, no. S268, p. 291-299. Cambridge University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:296037
    Summary
    It is well known that stars orbited by giant planets have higher abundances of heavy elements when compared with average field dwarfs. A number of studies have also addressed the possibility that light element abundances are different in these stars. In this paper we will review the present status of these studies. The most significant trends will be discussed