The effect of evaporation on the evolution of close-in giant planets

We include the effect of evaporation in our evolutionary calculations of close-in giant planets, based on a recent model for thermal evaporation taking into account the XUV flux of the parent star (Lammer et al. 2003). Our analysis leads to the existence of a critical mass for a given orbital distance m(crit)(a) below which the evaporation timescale becomes shorter than the thermal timescale of the planet. For planets with initial masses below m(crit), evaporation leads to a rapid expansion of the outer layers and of the total planetary radius, speeding up the evaporation process. Consequently, the planet does not survive as long as estimated by a simple application of mass loss rates without following consistently its evolution. We find out that the transit planet HD 209458b might be in such a dramatic phase, although with an extremely small probability. As a consequence, we predict that, after a certain time, only planets above a value M-crit(a) should be present at an orbital distance a of a star. For planets with initial masses above M-crit, evaporation does not affect the evolution of the radius with time.