Tidal Dissipation in Giant Planets
Abstract
Tidal interactions between moons and planets can have major effects on the orbits, spins, and thermal evolution of the moons. In the Saturn system, tidal dissipation in the planet transfers angular momentum from Saturn to the moons, causing them to migrate outwards. The rate of migration is determined by the mechanism of dissipation within the planet, which is closely tied to the planet's uncertain structure. We review current knowledge of giant planet internal structure and evolution, which has improved thanks to data from the \textit{Juno} and \textit{Cassini} missions. We discuss general principles of tidal dissipation, describing both equilibrium and dynamical tides, and how dissipation can occur in a solid core or a fluid envelope. Finally, we discuss the possibility of resonance locking, whereby a moon can lock into resonance with a planetary oscillation mode, producing enhanced tidal migration relative to classical theories, and possibly explaining recent measurements of moon migration rates.
Cite
@article{arxiv.2402.05338,
title = {Tidal Dissipation in Giant Planets},
author = {Jim Fuller and Tristan Guillot and Stephane Mathis and Carl Murray},
journal= {arXiv preprint arXiv:2402.05338},
year = {2024}
}
Comments
Accepted for Space Science Reviews. Chapter in the book based on the ISSI workshop "New Vision of the Saturnian System in the Context of a Highly Dissipative Saturn" (9-13 May 2022)