Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p31b1247c&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #P31B-1247
Physics
[5430] Planetary Sciences: Solid Surface Planets / Interiors, [5440] Planetary Sciences: Solid Surface Planets / Magnetic Fields And Magnetism, [6221] Planetary Sciences: Solar System Objects / Europa, [6281] Planetary Sciences: Solar System Objects / Titan
Scientific paper
Observations from the Galileo and Cassini spacecraft suggest that subsurface global water oceans are likely present on multiple icy satellites of Jupiter and Saturn. However, the dynamics of these oceans, under the influence of a time-varying tidal potential and buoyancy and coriolis forces, have not been investigated in detail. We have investigated the large scale ocean flow in two ways. First, we simulate the 3-D global circulation of the subsurface oceans on Europa and Titan driven primarily by a time-varying tidal potential and secondarily by heating at the base of the ocean. Second, we analyze the behavior of tidally-forced subsurface oceans in two-dimensions using quasi-nonlinear shallow water theory. These approaches allow us to predict potentially observable effects, in particular non-synchronous rotation of the ice shell driven by ocean torques and spatial variations in the heat flow supplied to the base of the ice shell, and magnetic induction effects due to the ocean circulation. Time-series analyses suggest that the ocean responds primarily at the tidal frequency; however, there are responses at lower frequencies as well. Preliminary results of full 3-D simulations will be presented, and comparisons will be made to the forced shallow water model.
Chen E. M.
Glatzmaier Gary A.
Nimmo Francis
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