The tidal excitation of r modes in a solar type star orbited by a giant planet companion and the effect on orbital evolution I: The aligned case

It has been suggested that tidal interaction is important for shaping the orbital configurations of close orbiting giant planets. The excitation of propagating waves and normal modes (dynamical tide) will be important for estimating time scales for orbital evolution. We consider the tidal interactio...

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Bibliographic Details
Published inarXiv.org
Main Authors Papaloizou, J C B, Savonije, G J
Format Paper Journal Article
LanguageEnglish
Published Ithaca Cornell University Library, arXiv.org 01.02.2023
Subjects
Angular momentum
Centrifugal force
Coriolis force
Evolution
Excitation
Extrasolar planets
Gas giant planets
Jupiter
Orbital mechanics
Orbital resonances (celestial mechanics)
Physics - Earth and Planetary Astrophysics
Physics - Solar and Stellar Astrophysics
Propagation modes
Resonance
Spherical harmonics
Stellar winds
Wave propagation
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Summary:It has been suggested that tidal interaction is important for shaping the orbital configurations of close orbiting giant planets. The excitation of propagating waves and normal modes (dynamical tide) will be important for estimating time scales for orbital evolution. We consider the tidal interaction of a Jupiter mass planet orbiting a solar type primary. Tidal and rotational frequencies are assumed comparable making the effect of rotation important. Although centrifugal distortion is neglected, Coriolis forces are fully taken into account. We focus in detail on the potentially resonant excitation of \(r\) modes associated with spherical harmonics of degrees three and five. These are mostly sited in the radiative core but with a significant response in the convective envelope where dissipation occurs. Away from resonance significant orbital evolution over the system lifetime is unlikely. However, tidal interaction is enhanced near resonances and the orbital evolution accelerated as they are passed through. This speed up may be sustained if near resonance can be maintained. For close orbits with primaries rotating sufficiently rapidly, this could arise from angular momentum loss and stellar spin down through a stellar wind bringing about significant orbital evolution over the system lifetime.
ISSN:2331-8422
DOI:10.48550/arxiv.2302.00473