期刊
ASTRONOMY & ASTROPHYSICS
卷 419, 期 2, 页码 L13-L16出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20040129
关键词
planetary systems; stars : individual : HD 209458; OGLE-TR-56
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.
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