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Anelastic Tidal Dissipation in Multi-Layer Planets

Published online by Cambridge University Press:  29 April 2014

Françcoise Remus ,
Stéphane Mathis ,
Jean-Paul Zahn  and
Valéry Lainey
Françcoise Remus
Affiliation:
LUTH, Observatoire de Paris – CNRS – Université Paris Diderot, 5 place Jules Janssen, F-92195 Meudon Cedex, France email: [email protected], [email protected] IMCCE, Observatoire de Paris – UMR 8028 du CNRS – Université Pierre et Marie Curie 77 avenue Denfert-Rochereau, F-75014 Paris, France email: [email protected] Laboratoire AIM Paris-Saclay, CEA/DSM – CNRS – Université Paris Diderot, IRFU/SAp Centre de Saclay, F-91191 Gif-sur-Yvette, France email: [email protected]
Stéphane Mathis
Affiliation:
Laboratoire AIM Paris-Saclay, CEA/DSM – CNRS – Université Paris Diderot, IRFU/SAp Centre de Saclay, F-91191 Gif-sur-Yvette, France email: [email protected]
Jean-Paul Zahn
Affiliation:
LUTH, Observatoire de Paris – CNRS – Université Paris Diderot, 5 place Jules Janssen, F-92195 Meudon Cedex, France email: [email protected], [email protected]
Valéry Lainey
Affiliation:
IMCCE, Observatoire de Paris – UMR 8028 du CNRS – Université Pierre et Marie Curie 77 avenue Denfert-Rochereau, F-75014 Paris, France email: [email protected]
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Abstract

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Earth-like planets have anelastic mantles, whereas giant planets may have anelastic cores. As for the fluid parts, the tidal dissipation of these regions, gravitationally perturbed by a companion, highly depends on its internal friction and thus its internal structure. Therefore, modeling this kind of interaction presents a high interest to constrain planetary interiors, whose properties are still quite uncertain. Here, we examine the anelastic tidal dissipation in deep planetary interiors, in presence of a fluid envelope, and taking into account its dependence on the rheology.

Taking plausible values for the anelastic parameters, and discussing the frequency-dependence of the anelastic dissipation, we show how this mechanism may compete with the dissipation in fluid layers, when applied to Jupiter- and Saturn-like planets. We also discuss the case of the icy giants Uranus and Neptune. Finally, we show how the results may be implemented to describe the dynamical evolution of planetary systems.

Keywords

planets and satellites: general(stars:) planetary systems
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 362 - 368
Copyright
Copyright © International Astronomical Union 2014 

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