@SCV95) with a solar or non-solar enrichment in heavy elements described by the appropriate EOS’s [@BCB08]. In the present calculations, our fiducial model consists of a planet with a central core made up of water, with the ANEOS EOS [@TL72]. A detailed analysis of the effects of different EOS’s, core compositions and heavy material repartitions within the planet can be found in @BCB08, as well as a comparison with models from other groups, in particular the ones by @FMB07.

Transiting planets are by definition very close to their host star ($a< 0.1$AU). In that case, the stellar irradiation strongly affects the planet atmospheric structure to deep levels [@BHA01] and thus the planet’s evolution (@GBH96, @BCB03, @BSH03, @CBB04). We use a grid of irradiated atmosphere models based on the calculations of [@BHA01], computed for different levels of stellar irradiation relevant to the present study. For planets with a finite orbital eccentricity, the mean stellar flux received is given by: $$\label{finc}
<F_{\mathrm{inc}}> =f\, R_\star^2\  \sigma  T_{\mathrm{eff},\star}^4<\frac{1}{r^2} >= f\,\left( \frac{R_\star}{a } \right)^2 \frac{\sigma T_{\mathrm{eff},\star}^4}{\sqrt{1-e^2}}\,,$$ where $\Rs$ and $T_{\mathrm{eff},\star}$ are the stellar radius and effective temperature, $\sigma$ the Stefan-Boltzmann constant, $a$ and $e$ the orbital semi-major axis and eccentricity and $f$ is a geometrical 