EDP Sciences
Free Access
Issue
A&A
Volume 402, Number 2, May I 2003
Page(s) 701 - 712
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361:20030252
Published online 14 April 2003


A&A 402, 701-712 (2003)
DOI: 10.1051/0004-6361:20030252

Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458

I. Baraffe1, 2, G. Chabrier1, T. S. Barman3, F. Allard1 and P. H. Hauschildt4

1  C.R.A.L (UMR 5574 CNRS), École Normale Supérieure, 69364 Lyon Cedex 07, France
    e-mail: ibaraffe,chabrier,fallard@ens-lyon.fr
2  Max-Planck-Institut für Astrophysik, Karl-Schwarzschildstr.1, 85748 Garching, Germany
3  Department of Physics, Wichita State University, Wichita, KS 67260-0032, USA
    e-mail: travis.barman@wichita.edu
4  Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
    e-mail: phauschildt@hs.uni-hamburg.de

(Received 27 November 2002 / Accepted 18 February 2003 )

Abstract
We present evolutionary models for cool brown dwarfs and extra-solar giant planets. The models reproduce the main trends of observed methane dwarfs in near-IR color-magnitude diagrams. We also present evolutionary models for irradiated planets, coupling for the first time irradiated atmosphere profiles and inner structures. We focus on HD 209458-like systems and show that irradiation effects can substantially affect the radius of sub-jovian mass giant planets. Irradiation effects, however, cannot alone explain the large observed radius of HD 209458b. Adopting assumptions which optimise irradiation effects and taking into account the extension of the outer atmospheric layers, we still find ~20% discrepancy between observed and theoretical radii. An extra source of energy seems to be required to explain the observed value of the first transit planet.


Key words: planetary systems -- stars: brown dwarfs -- stars: evolution -- stars: individual (HD 209458)

Offprint request: I. Baraffe, ibaraffe@ens-lyon.fr

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© ESO 2003

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