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Article Dans Une Revue Astronomy and Astrophysics - A&A Année : 2004

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

Franck Selsis
  • Fonction : Auteur
T. S. Barman
  • Fonction : Auteur
France Allard
P. H. Hauschildt
  • Fonction : Auteur
H. Lammer
  • Fonction : Auteur

Résumé

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 $m_{\\rm crit}(a)$ below which the evaporation timescale becomes shorter than the thermal timescale of the planet. For planets with initial masses below $m_{\\rm crit}$, 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 $m_{\\rm crit}(a)$ should be present at an orbital distance $a$ of a star. For planets with initial masses above $m_{\\rm crit}$, evaporation does not affect the evolution of the radius with time.

Dates et versions

hal-00008486 , version 1 (06-09-2005)

Identifiants

Citer

Isabelle Baraffe, Franck Selsis, Gilles Chabrier, T. S. Barman, France Allard, et al.. The effect of evaporation on the evolution of close-in giant planets. Astronomy and Astrophysics - A&A, 2004, 419, pp.L13-L16. ⟨hal-00008486⟩
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