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Volatiles and refratories in solar analogs: No terrestial planet connection

Published online by Cambridge University Press:  10 November 2011

Jonay I. González Hernández ,
Garik Israelian ,
Nuno C. Santos ,
Sergio Sousa ,
Elisa Delgado-Mena ,
Vasco Neves  and
Stéphane Udry
Jonay I. González Hernández
Affiliation:
Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, 38200 La Laguna, Spain email: jonay@iac.es Dpto. de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
Garik Israelian
Affiliation:
Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, 38200 La Laguna, Spain email: jonay@iac.es
Nuno 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
Sergio Sousa
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
Elisa Delgado-Mena
Affiliation:
Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, 38200 La Laguna, Spain email: jonay@iac.es
Vasco Neves
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
Stéphane Udry
Affiliation:
Observatoire Astronomique de l'Université de Genève, 51 Ch. des Maillettes, -Sauverny- Ch1290, Versoix, Switzerland
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Abstract

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We have analysed very high-quality HARPS and UVES spectra of 95 solar analogs, 24 hosting planets and 71 without detected planets, to search for any possible signature of terrestial planets in the chemical abundances of volatile and refractory elements with respect to the solar abundances.

We demonstrate that stars with and without planets in this sample show similar mean abundance ratios, in particular, a sub-sample of 14 planet-host and 14 “single” solar analogs in the metallicity range 0.14 < [Fe/H] < 0.36. In addition, two of the planetary systems in this sub-sample, containing each of them a super-Earth-like planet with masses in the range ~ 7-11 Earth masses, have different volatile-to-refratory abundance ratios to what would be expected from the presence of a terrestial planets.

Finally, we check that after removing the Galactic chemical evolution effects any possible difference in mean abundances, with respect to solar values, of refratory and volatile elements practically dissappears.

Keywords

stars: abundancesstars: fundamental parametersplanetary systemsplanetary systems: formationstars: atmospheres
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 422 - 423
Copyright
Copyright © International Astronomical Union 2011

References

González Hernández, J. I., Israelian, G., Santos, N. C., et al. 2010, ApJ, 720, 1592CrossRefGoogle Scholar
Kurucz, R. L. ATLAS9 Stellar Atmospheres Programs and 2 km s−1 Grid, CD-ROM No. 13, Smithsonian Astrophysical Observatory, Cambridge, 1993Google Scholar
Meléndez, J., Asplund, M., Gustafsson, B., & Yong, D. 2009, ApJ Letters, 704, L66CrossRefGoogle Scholar
Neves, V., Santos, N. C., Sousa, S. G., Correia, A. C. M., & Israelian, G. 2009, A&A, 497, 563Google Scholar
Ramírez, I., Meléndez, J., & Asplund, M. 2009, A&A Letters, 508, L17Google Scholar
Ramírez, I., Asplund, M., Baumann, P., Meléndez, J., & Bensby, T. 2010, A&A, 521, A33Google Scholar
Sousa, S. G., et al. 2008, A&A, 487, 373Google Scholar
Sneden, C. 1973, PhD Dissertation, Univ. of Texas, AustinGoogle Scholar
Udry, S. & Santos, N. C. 2007, ARA&A, 45, 397Google Scholar