A Mass Function Constraint on Extrasolar Giant Planet Evaporation Rates

Details A Mass Function Constraint on Extrasolar Giant Planet Evaporation Rates A Mass Function Constraint on Extrasolar Giant Planet Evaporation Rates

2007-02-09

arxiv.org/abs/astro-ph/0702276v1

Astrophys.J.658:L59-L62,2007

Astronomy and Astrophysics

Astrophysics

accepted by Astrophys. J. Letters on 1 February 2007

Scientific paper

10.1086/513422

The observed mass function for all known extrasolar giant planets (EGPs) varies approximately as M^{-1} for mass M between 0.2 Jupiter masses (M_J) and 5 M_J. In order to study evaporation effects for highly-irradiated EGPs in this mass range, we have constructed an observational mass function for a subset of EGPs in the same mass range but with orbital radii <0.07 AU. Surprisingly, the mass function for such highly-irradiated EGPs agrees quantitatively with the M^{-1} law, implying that the mass function for EGPs is preserved despite migration to small orbital radii. Unless there is a remarkable compensation of mass-dependent orbital migration for mass-dependent evaporation, this result places a constraint on orbital migration models and rules out the most extreme mass loss rates in the literature. A theory that predicts more moderate mass loss gives a mass function that is closer to observed statistics but still disagrees for M < 1 M_J.

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