Mathematics – Logic
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.2402h&link_type=abstract
American Astronomical Society, DPS meeting #38, #24.02; Bulletin of the American Astronomical Society, Vol. 38, p.521
Mathematics
Logic
Scientific paper
Tidal dissipation is one of the possibilities to explain the geologic activity on Enceladus observed during close Cassini-flybys (Porco et al., Science 311, 2006). From Cassini observations the power needed to drive the satellite's thermal activity is estimated to range between 3.9 and 7.7 GW (Spencer et al., Science 311, 2006). However, Enceladus' inner neighboring moon Mimas shows a heavily cratered surface without signs of geological activity for billions of years. In the present study we calculate tidal dissipation rates for a layered satellite based on the assumption of a Maxwell rheological model. Since tidal dissipation rates also depend on the interior structure, which is not well-constrained, we compare homogeneous models to more complex ones including possible differentiation and the presence of a liquid water layer underneath an icy crust. Such models are applied to Enceladus and Mimas, which is exposed to stronger tidal deformation due to its orbital characteristics, mainly its larger eccentricity and mean motion. The Maxwell rheological model is considered as a useful approximation for modeling the cold state of Mimas. However, it may be questionable for Enceladus in view of the low viscosities caused by higher internal temperatures. Therefore, we discuss other rheological concepts to account even for a partially molten state of the interior. Since tidal dissipation implies a loss in orbital energy it has a major impact on the orbital evolution of the satellites. For the calculated dissipation rates we investigate the consequences for the long-term orbital history of Mimas and Enceladus.
Grott Matthias
Hussmann Hauke
Sohl Frank
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