How Does Ice Shell Geometry Shape Ocean Dynamics on Icy Moons?

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Abstract
A poleward‐thinning ice shell can drive circulation in the subsurface oceans of icy moons by imposing a meridional temperature gradient–colder at the equator than the pole–through the freezing point suppression due to pressure. This temperature gradient sets a buoyancy gradient, whose sign depends on the thermal expansion coefficient determined by ocean salinity. Together with vertical mixing, this buoyancy forcing shapes key oceanic features, including zonal currents in thermal wind balance, baroclinic instability of those currents, meridional heat transport by eddies, and vertical stratification. We use high‐resolution numerical simulations to explore how variations in ice shell thickness affect these processes. Our simulations span a wide range of topographic slopes, pole‐to‐equator temperature differences, and vertical mixing strengths, for both fresh and salty oceans. We find that baroclinic eddies dominate large‐scale circulation and meridional heat transport, consistent with studies assuming a flat ice‐ocean interface. However, sloped topography introduces new effects: when lighter water overlies denser water along the slope, circulation weakens as a stratified layer thickens beneath the poles. Conversely, when denser water lies beneath the poles, circulation strengthens as topography increases the available potential energy. We develop a scaling framework that predicts heat transport and stratification across all simulations. Applying this framework to Enceladus, Europa, and Titan, we infer ocean heat fluxes, stratification, and tidal energy dissipation, showing large‐scale circulation constrains tidal heating and links future observations of ice thickness and rotation to subsurface ocean dynamics.
Funding Information
  • NASA Astrobiology Institute (80NSSC19K1427)

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