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On icy worlds, the ice shell and subsurface ocean form a coupled system --heat and salinity flux from the ice shell induced by the ice thickness gradientdrives circulation in the ocean, and in turn, the heat transport by oceancirculation shapes the ice shell. Therefore, understanding the dependence ofthe efficiency of ocean heat transport (OHT) on orbital parameters may allow usto predict the ice shell geometry before direct observation is possible,providing useful information for mission design. Inspired by previous works onbaroclinic eddies, I first derive scaling laws for the OHT on icy moons, drivenby ice topography, and then verify them against high resolution 3D numericalsimulations. Using the scaling laws, I am then able to make predictions for theequilibrium ice thickness variation knowing that the ice shell should be closeto heat balance. Ice shell on small icy moons (e.g., Enceladus) may developstrong thickness variations between the equator and pole driven by thepolar-amplified tidal dissipation in the ice, to the contrary, ice shell onlarge icy moons (e.g., Europa, Ganymede, Callisto etc.) tends to be flat due tothe smoothing effects of the efficient OHT. These predictions are manifested bythe different ice evolution pathways simulated for Enceladus and Europa,considering the ice freezing/melting induced by ice dissipation, conductiveheat loss and OHT as well as the mass redistribution by ice flow.

Different ice shell geometries on Europa and Enceladus due to their different sizes: impacts of ocean heat transport