Close-in exoplanets experience very strong stellar irradiation. These planets indeed orbit at semi-major axis shorter than 0.1 AU. If they are in synchronous rotation -- as they are expected since the strong tidal forces from the star quickly synchronize the planet -- the difference of temperature between the constantly exposed day side and the night side should lead to intense atmospheric dynamics. For larger semi-major axis, the differential rotation as well as the eventual eccentricity generate a time-varying incoming flux from the star for each atmospheric parcel.
In that framework, it is not strange that static models have difficulties to reproduce or explain some observational constraints. A time-dependent radiative transfer model is essential in order to understand the extrasolar planets atmospheric structure. Moreover, coupled radiative transfer method and hydrodynamical code are required to fully understand and analyze these exoplanets under strong stellar irradiation.
I will discuss the problems of time-dependency in exoplanets atmosphere and present a model where some of the issues are taken into account.
2013 July 25, 13:30
Centro de AstrofÝsica da Universidade do Porto (Auditorium)
Rua das Estrelas, 4150-762 Porto