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Tidal Deformation and Dissipation Processes in Icy Worlds.
G Tobie1, P Auclair-Desrotour2, M Běhounková3
1Laboratoire de Planétologie et Géosciences, UMR 6112, CNRS, Nantes Université, Université d'Angers, Le Mans Université, Nantes, France.
Space Science Reviews
|January 20, 2025
Summary
Tidal forces drive activity on icy moons like Europa and Enceladus by deforming their internal layers and generating heat. Understanding these tidal interactions is key to explaining their geological activity and internal structure.
Area of Science:
- Planetary Science
- Geophysics
- Astrobiology
Background:
- Tidal interactions are crucial for the dynamics and evolution of icy worlds.
- Tidal heating is a primary driver of geological activity on moons like Europa and Enceladus.
- The precise mechanisms of tidal deformation and heat generation remain poorly understood.
Purpose of the Study:
- To review methods for computing tidal deformation and dissipation in icy moons.
- To analyze how tidal forces affect different internal layers (core, ocean, ice shell).
- To explore the link between tidal heating, internal evolution, and surface activity.
Main Methods:
- Review of theoretical models for tidal deformation and dissipation.
- Analysis of visco-elastic tidal response using various rheological models.
- Examination of dissipation processes in different planetary layers.
Main Results:
- Tidal forcing varies with orbital parameters, significantly impacting the internal heat budget over time.
- Tidal deformation can reveal interior structure, particularly the hydrosphere.
- Tidal heating can lead to internal melting and diverse surface activities.
Conclusions:
- Tidal deformation and dissipation are critical factors in the evolution and activity of icy moons.
- Future missions can use tidal response data to constrain interior structures and activity.
- Understanding tidal interactions is essential for assessing the habitability of ocean worlds.
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