Implications Of Shallow-shell Models For Topographic Relaxation On Icy Satellites

Icy satellites host topography at many length scales, from rifts and craters on the small end to equatorial-pole shell thickness differences that are comparable to these bodies’ circumference.

The rate of topographic evolution depends on the rheology of the ice shell, the difference in density between the shell and potential global subsurface oceans, the ice shell thickness distribution, as well as the rate of tidal heat dissipation in the shell.

Here we analyze relaxation of topography starting from the Stokes equations for viscous fluid flow. We write out the shallow-shell models (with and without a rigid crust) and compare the resulting time scales to previous work.

Using three-dimensional linearized flow for small-amplitude topographic perturbations, we recover the time scales of relaxation from the shallow models as well as shells that are not shallow. For a shell of constant viscosity, we find that the topographic relaxation time scale is constant for wavelengths larger than the ice thickness, an idea that runs contrary to the existing paradigm.

For a shell with a viscosity that decreases exponentially with depth, we show numerically that there is a regime where the larger viscosity outer crust acts as a nearly rigid boundary. In this case, the relaxation time scale depends on the wavelength. For the largest spatial scales, the time scale becomes independent of wavelength again and the value is set by the average shell viscosity.

However, the spatial scale that this transition occurs at becomes larger as the viscosity contrast increases, limiting the applicability of the scale-independent relaxation rate. These results for the relaxation of topography have implications for interpreting relaxed crater profiles, inferences of ice shell thickness from topography, and upcoming observations from missions to the outer solar system.

Colin R. Meyer, Aaron G. Stubblefield, Brent M. Minchew, Samuel S. Pegler, Alexander Berne, Jacob J. Buffo, Tara C. Tomlinson

Comments: 16 pages, 5 figures
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Fluid Dynamics (physics.flu-dyn)
Cite as: arXiv:2504.20095 [astro-ph.EP] (or arXiv:2504.20095v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2504.20095
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Submission history
From: Colin Meyer
[v1] Sat, 26 Apr 2025 01:34:25 UTC (1,516 KB)
https://arxiv.org/abs/2504.20095

Astrobiology, Astrogeology,