Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p22b..06t&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P22B-06
Physics
[6218] Planetary Sciences: Solar System Objects / Jovian Satellites, [6280] Planetary Sciences: Solar System Objects / Saturnian Satellites, [6024] Planetary Sciences: Comets And Small Bodies / Interiors
Scientific paper
The tidal flow response and associated dissipative heat generated in a satellite ocean depends strongly on the ocean configuration parameters as these parameters control the form and frequencies of the ocean's natural modes of oscillation; if there is a near match between the form and frequency of one of these natural modes and that of one of the available tidal forcing constituents, the ocean can be resonantly excited, producing strong tidal flow and appreciable dissipative heat generation. Of primary interest in this study are the ocean parameters that can be expected to evolve (notably, the ocean depth in an ocean attempting to freeze, and the stratification in an ocean attempting to cool) because this evolution can cause an ocean to be pushed into a resonant configuration where the increased dissipative heat of the resonant response halts further evolution and a liquid ocean can be maintained by ocean tidal heat. In this case the resonant ocean tidal response is not only allowed but may be inevitable. Previous work on this topic is extended to describe the resonant configurations in both unstratified and stratified oceans on Europa, Ganymede, Callisto, Enceladus, and Titan under free-surface assumptions (expected to be applicable on thin ice-cover oceans such as Europa) as well as the alternative situation where the ocean is expected to be constrained by a thick ice layer (e.g. Ganymede). It is shown that plausible scenarios are available that provide for each of these satellites having moved into a resonant state involving strong ocean tides and elevated heat generation.
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