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            <title xml:lang="en">Modeling the atmosphere of extrasolar giant planets</title>
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                <title xml:lang="en">Modeling the atmosphere of extrasolar giant planets</title>
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                <term xml:lang="en">extrasolar planets radiative tranfer HD209458b</term>
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              <p>The discovery of the first extrasolar planet transiting its star, HD209458b, provides new informations on this kind of objects : the Pegasides. However, static radiative models of atmosphere fail to explain the constraints inferred on on its radius and atmospheric composition (ref. Charbonneau et al. 2002). We developed a radiative model for the atmosphere of the Pegasides. A static case was first built. We determined a mean thermal structure for HD209458b and its atmospheric composition. We confirmed the important role of alkali metals in the thermal balance of Pegasides. In a second step, we introduced a rotation of the atmosphere mimicking a constant-with-height zonal wind. The zonal wind yields temperature contrasts which can explain the observations of Charbonneau et al. (2002). More generally, we studied the role of some parameters such as the planet-to-star distance or the wind velocity.</p>
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              <p>La découverte d'une première planète extrasolaire transitant devant son étoile, HD209458b, a fourni de nouvelles informations sur ce type d'objets : les Pégasides. Toutefois, les modèles radiatifs statiques d'atmosphère peinent à expliquer les premières contraintes obtenues sur son rayon et sa composition (réf. Charbonneau et al. 2002). Nous avons développé un modèle radiatif pour l'atmosphère de ces Pégasides. Un cas statique a d'abord été construit. Nous avons déterminé une structure thermique moyenne pour HD209458b et sa composition atmosphérique. Nous avons entre autres confirmé le rôle de l'absorption par les alcalins dans les Pégasides. Nous avons ensuite introduit une rotation de l'atmosphère simulant un vent zonal constant avec l'altitude. Les vents zonaux engendrent des contrastes thermiques pouvant expliquer les observations de Charbonneau et al. (2002). Nous avons aussi étudié plus généralement le rôle des paramètres comme la distance planète-étoile ou la vitesse du vent.</p>
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