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Li and Be Depletion in Stars with Exoplanets?

Published online by Cambridge University Press:  23 April 2012

E. Delgado Mena ,
G. Israelian ,
J. I. González Hernández ,
R. Rebolo ,
N. C. Santos ,
S. G. Sousa  and
J. Fernandes
E. Delgado Mena
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain.
G. Israelian
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain.
J. I. González Hernández
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain.
R. Rebolo
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: edm@iac.es Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain. Consejo Superior de Investigaciones Científicas, 28006, Madrid, Spain
N. C. Santos
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal. Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal.
S. G. Sousa
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal. Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal.
J. Fernandes
Affiliation:
Centro de Física Computacional, Universidade de Coimbra, Portugal.
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Abstract

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It is well known that stars with orbiting giant planets have a higher metallic content than stars without detected planets. In addition, we have found that solar-type stars with planets present an extra Li depletion when compared with field stars. On the other hand, Be needs a greater temperature to be destroyed, so we may find such a relation in cooler stars, whose convective envelopes are deep enough to carry material to layers where Be can be burned. We present Li and Be abundances for an extensive sample of stars with and without detected planets, covering a wide range of effective temperatures (4700-6500 K) with the aim of studying possible differences between the abundances of both groups. The processes that take place in the formation of planetary systems may affect the mixing of material inside their host stars and hence the abundances of light elements.

Keywords

stars: abundances — stars: atmospheres — stars: fundamental parameters — stars: planetary systems — stars: planetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 466 - 467
Copyright
Copyright © International Astronomical Union 2012

References

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