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Metallicity of M dwarfs: The link to exoplanets

Published online by Cambridge University Press:  10 November 2011

V. Neves ,
X. Bonfils  and
N. C. Santos
V. Neves
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal email: vasco.neves@astro.ua.pt Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, F-38041 Grenoble Cédex 9, France
X. Bonfils
Affiliation:
Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, F-38041 Grenoble Cédex 9, France
N. C. Santos
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal email: vasco.neves@astro.ua.pt Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal
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Abstract

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The determination of the stellar parameters of M dwarfs is of prime importance in the fields of galactic, stellar and planetary astronomy. M stars are the least studied galactic component regarding their fundamental parameters. Yet, they are the most numerous stars in the galaxy and contribute to most of its total (baryonic) mass. In particular, we are interested in their metallicity in order to study the star-planet connection and to refine the planetary parameters. As a preliminary result we present a test of the metallicity calibrations of Bonfils et al. (2005), Johnson & Apps (2009), and Schlaufman & Laughlin (2010) using a new sample of 17 binaries with precise V band photometry.

Keywords

stars: fundamental parametersplanetary systemsstars: late-typestars: abundancesstars: 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. 443 - 444
Copyright
Copyright © International Astronomical Union 2011

References

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Schlaufman, K. C. & Laughlin, G. 2010, A&A, 519, A105Google Scholar
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