Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458
Baraffe, Isabelle Chabrier, Gilles Barman, Travis S. Allard, France Hauschildt, Peter H.
Baraffe, Isabelle
Chabrier, Gilles
Barman, Travis S.
Allard, France
Hauschildt, Peter H.
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2003-04-14
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Article
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Planetary Systems,Stars: Brown Dwarfs,Stars: Evolution,Stars: Individual (hd 209458),Infrared Radiation,Irradiation,Mathematical Models,Planets,Solar Energy,Planetry Systems,Astrophysics
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Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458 I. Baraffe, G. Chabrier, T. S. Barman, F. Allard and P. H. Hauschildt A&A, 402 2 (2003) 701-712 DOI: https://doi.org/10.1051/0004-6361:20030252
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. © 2018 Elsevier B.V., All rights reserved.
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This is an open access article under the CC BY license.
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EDP Sciences
Journal
Astronomy and Astrophysics
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0004-6361
1432-0746
1432-0746