Volume 462, Number 1, January IV 2007
|Page(s)||L5 - L8|
|Published online||29 November 2006|
Letter to the Editor
Tidal dissipation within hot Jupiters: a new appraisal
Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR 8028, 77 Avenue Denfert-Rochereau, 75014 Paris, France e-mail: email@example.com
2 École Normale Supérieure de Lyon, Centre de Recherche Astronomique de Lyon, 46 allée d'Italie, 69364 Lyon Cedex 07, CNRS UMR 5574, Université de Lyon 1, France
3 Departamento de Física da Universidade de Aveiro, Campus Universitário de Santiago, 3810-193 Aveiro, Portugal
Accepted: 22 November 2006
Context.Eccentricity or obliquity tides have been proposed as the missing energy source that may explain the anomalously large radius of some transiting “hot Jupiters”. To maintain a non-zero and large obliquity, it was argued that the planets can be locked in a Cassini state, i.e. a resonance between spin and orbital precessions.
Aims.We compute the tidal heating within “inflated” close-in giant planets with a non-zero eccentricity or obliquity. We further inspect whether the spin of a “hot Jupiter” could have been trapped and maintained in a Cassini state during its early despinning and migration.
Methods.We estimate the capture probability in a spin-orbit resonance between ~0.5 AU (a distance where tidal effects become significant) and 0.05 AU for a wide range of secular orbital frequencies and amplitudes of gravitational perturbations. Numerical simulations of the spin evolution are performed to explore the influence of tidal despinning and migration processes on the resonance stability.
Results.We find that tidal heating within a non-synchronous giant planet is about twice larger than previous estimates based on the hypothesis of synchronization. Chances of capture in a spin-orbit resonance are very good around 0.5 AU but they decrease dramatically with the semi-major axis. Furthermore, even if captured, both tidal despinning and migration processes cause the tidal torque to become large enough that the obliquity ultimately leaves the resonance and switches to near .
Conclusions.Locking a “hot Jupiter” in an isolated spin-orbit resonance is unlikely at 0.05 AU but could be possible at larger distances. Another mechanism is then required to maintain a large obliquity and create internal heating through obliquity tides.
Key words: planets and satellites: formation / celestial mechanics / gravitation
© ESO, 2007
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