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Precise characterisation of exoplanet-host stars parameters

Published online by Cambridge University Press:  10 November 2011

Sylvie Vauclair
Sylvie Vauclair*
Affiliation:
Institut de Recherches en Astrophysique et Planetologie, 14 avenue Edouard Belin, 31400, Toulouse, France email: sylvie.vauclair@ast.obs-mip.fr
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Abstract

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Studying the internal structure of exoplanet-host stars compared to that of similar stars without detected planets is particularly important for the understanding of planetary formation. In this framework, asteroseismic studies represent an excellent tool for a better characterization of stars and for a precise determination of the stellar parameters like mass, radius, gravity, effective temperature. The detection of stellar oscillations is obtained with the same instruments as used for the discovery of exoplanets, both from the ground and from space, although the time scales are very different. Here I discuss some details about the characterization of exoplanethost stars from seismology and the importance of the helium and heavy element abundances in this respect.

Keywords

stars: abundancesstars: oscillationsstars: interiors
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. 30 - 33
Copyright
Copyright © International Astronomical Union 2011

References

Bazot, M. & Vauclair, S. 2004, A&A, 427, 965Google Scholar
Bazot, M., Vauclair, S., Bouchy, F., & Santos, N. 2005, A&A, 440, 615Google Scholar
Ballot, J., Gizon, L., et al. 2011 in preparationGoogle Scholar
Bouchy, F., Bazot, M., Santos, N., Vauclair, S., & Sosnowska, D. 2005, A&A, 440, 609Google Scholar
Castro, M. & Vauclair, S. 2006, A&A, 456, 611Google Scholar
Lebreton, Y., Fernandes, J., & Lejeune, T. 2001, A&A, 374, 540Google Scholar
Mayor, M. & Queloz, D. 1995, Nature, 78, 355CrossRefGoogle Scholar
Metcalfe, T. S., Monteiro, M. J. P. F. G., Thompson, M. J. et al. 2010, ApJ, 723, 1583CrossRefGoogle Scholar
Roxburgh, I. W., & Vorontsov, S. V. 1994, MNRAS, 267, 297CrossRefGoogle Scholar
Roxburgh, I. W. 2007, MNRAS, 379, 801CrossRefGoogle Scholar
Santos, N. C., Israelian, G., & Mayor, M. 2004, A&A, 415, 1153Google Scholar
Santos, N. C., Israelian, G., Mayor, M., Bento, J. P., Almeida, P. C., Sousa, S. G., & Ecuvillon, A. 2005, A&A, 437, 1127Google Scholar
Silvotti, R., Schuh, S., Janulis, R., et al. 2007, Nature, 449, 189CrossRefGoogle Scholar
Soriano, M., Vauclair, S., Vauclair, G., & Laymand, M. 2007, A&A, 471, 885Google Scholar
Soriano, M. & Vauclair, S. 2008, A&A, 488, 975Google Scholar
Soriano, M. & Vauclair, S. 2010, A&A, 513, 49Google Scholar
Vauclair, S. 2004, ApJ, 605, 874CrossRefGoogle Scholar
Vauclair, S. & Théado, S. 2004, A&A, 425, 179Google Scholar
Vauclair, S., Laymand, M., Bouchy, F., Vauclair, G., Hui Bon Hoa, A., Charpinet, S., & Bazot, M. 2008, A&A, 482, L5Google Scholar