Ocean Dynamics of Outer Solar System Satellites

Ocean worlds are prevalent in the solar system. Focusing on Enceladus, Titan, Europa, and Ganymede, I use rotating convection theory and numerical simulations to predict ocean currents and the potential for ice‐ocean coupling. When the influence of rotation is relatively strong, the oceans have multiple zonal jets, axial convective motions, and most efficient heat transfer at high latitudes. This regime is most relevant to Enceladus and possibly to Titan and may help explain their long‐wavelength topography. For a more moderate rotational influence, fewer zonal jets form, Hadley‐like circulation cells develop, and heat flux peaks near the equator. This regime is predicted for Europa, where it may help drive geologic activity via thermocompositional diapirism in the ice shell, and is possible for Titan. Weak rotational influence allows concentric zonal flows and overturning cells with no preferred orientation. Predictions for Ganymede's ocean span multiple regimes. Plain Language Summary The outer solar system is host to a large number of diverse satellites, many of which likely have global oceans beneath their outer icy shells. I use theoretical arguments and numerical models to make predictions about ocean currents and heat transfer across such oceans. Our results suggest that strong ocean currents exist in Enceladus, Titan, Europa, and Ganymede and cause the transfer of heat to vary with latitude that may modify the overlying ice shell. Key Points Ocean dynamics are important for the habitability of icy ocean worlds Strong ocean currents likely exist in Enceladus, Titan, Europa, and Ganymede Convective heat transfer in the ocean is predicted to vary with latitude, which would modify the thermophysical structure of the ice shell