Thermal Evolution of the mid-size Saturnian Satellites

Details Thermal Evolution of the mid-size Saturnian Satellites Thermal Evolution of the mid-size Saturnian Satellites

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p31d..05m&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P31D-05

Physics

6020 Ices, 6040 Origin And Evolution, 6099 General Or Miscellaneous, 6280 Saturnian Satellites, 8147 Planetary Interiors (5430, 5724, 6024)

Scientific paper

Thermal history models for the mid-sized Saturnian satellites Mimas, Enceladus, Tethys, Dione, Iapetus, and Rhea with radiogenic heating have been calculated assuming stagnant lid convection in undifferentiated satellites and varying parameter values over broad ranges. Of all satellites under consideration, only Dione, Rhea and Iapetus do show significant internal activities related to convective overturn for extended periods of time. The interiors of Mimas, Enceladus, and Tethys do not convect or do so only for brief periods of time early in their thermal histories. Although we use lower densities than previous models, our calculations suggest higher interior temperatures but also thicker rigid shells above the convecting regions. Temperatures in the stagnant lid will allow melting of ammonia-dihydrate. Dione, Rhea and Iapetus may differentiate early and form early oceans, Iapetus only if ammonia is present. Mimas, Enceladus, and Tethys with ammonia may differentiate if they accreted in an optically thick nebula with ambient temperatures around 250 K or if ^{26}Al is a releavant heat source. Our models suggest that the outer shells of the satellites are largely primordial in composition even if the satellites differentiated. In these cases the deep interior may be layered with a pure ice shell underlain by an ammonia dihydrate layer and a rock core.

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