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Atmospheres From Very Low-Mass Stars to Extrasolar Planets

Published online by Cambridge University Press:  30 November 2012

F. Allard ,
D. Homeier ,
B. Freytag  and
C.M. Sharp
F. Allard
Affiliation:
CRAL, UMR 5574, CNRS, Université de Lyon, École Normale Supérieure de Lyon, 46 allée d’Italie, 69364 Lyon Cedex 07, France;. e-mail: [email protected]
D. Homeier
Affiliation:
CRAL, UMR 5574, CNRS, Université de Lyon, École Normale Supérieure de Lyon, 46 allée d’Italie, 69364 Lyon Cedex 07, France;. e-mail: [email protected]
B. Freytag
Affiliation:
CRAL, UMR 5574, CNRS, Université de Lyon, École Normale Supérieure de Lyon, 46 allée d’Italie, 69364 Lyon Cedex 07, France;. e-mail: [email protected]
C.M. Sharp
Affiliation:
CRAL, UMR 5574, CNRS, Université de Lyon, École Normale Supérieure de Lyon, 46 allée d’Italie, 69364 Lyon Cedex 07, France;. e-mail: [email protected]
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Abstract

Within the next few years, several instruments aiming at imaging extrasolar planets will see first light. In parallel, low mass planets are being searched around red dwarfs which offer more favorable conditions – both for radial velocity detection and transit studies – than solar-type stars. We review recent advancements in modeling the stellar to substellar transition. The revised solar oxygen abundances and cloud models allow to reproduce the photometric and spectroscopic properties of this transition to a degree never achieved before, but problems remain at the stellar-brown dwarf transition typical of the Teff range of characterizable exoplanets.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 57: Low-Mass Stars and the Transition Stars/Brown Dwarfs - Evry Schatzman School on Stellar Physics XXIII , 2012 , pp. 3 - 43
Copyright
© EAS, EDP Sciences 2012

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