  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.
