, which is a ratio of buoyancy flux, moon rotation rate, and ocean depth—for which observational constraints do exist.
The authors present a series of simulations that explore a wide parameter range of ocean depth, moon rotation rate, and driving heat flux. In the small–Rossby number regime likely appropriate for icy moons, the simulated moon’s rate of rotation has a strong effect on the dynamics of the subsurface ocean. This stands in contrast to theConsistent with arguments rooted in well-understood rotating fluid dynamics in a spherical shell, the ocean’s circulation breaks into two regions.
According to the authors, turbulence created by the global convective process likely led to the creation of bands of alternating ocean currents, similar to the mechanism that generates the colorful zones and belts found in Jupiter’s atmosphere. In fact, the general circulation pattern found within the oceans of these outer solar system moons may bear remarkable similarity to that of the Jovian parent.
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