Thermal Evolution Models for Enceladus Defining the context for the formation of the South Pole thermal anomaly

Details Thermal Evolution Models for Enceladus Defining the context for the formation of the South Pole thermal anomaly Thermal Evolution Models for Enceladus Defining the context for the formation of the South Pole thermal anomaly

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p32a..05m&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #P32A-05

Other

3616 Hydrothermal Systems (0450, 1034, 3017, 4832, 8135, 8424), 5430 Interiors (8147), 5455 Origin And Evolution, 8424 Hydrothermal Systems (0450, 1034, 3017, 3616, 4832, 8135)

Scientific paper

We have developed thermal evolution models for Enceladus as a function of time of formation (i.e., initial amount of short-lived radiogenic species available), models for the cooling of the Saturnian nebula, silicate hydration, and presence of ammonia. Differentiation of the models is mainly determined by their time of formation with respect to the formation of CAIs. For each model we identify the times when thermal conditions are suitable for significant tidal dissipation heating to be initiated and sustained until the present. This defines the context for forming the South Pole thermal anomaly detected by Cassini instruments. This anomaly has been suggested to power a geyser that might be responsible for the origin of Saturn's E-ring. However, Enceladus' nonhydrostatic shape and its old surface indicate that the overall outer layer might be thick, thus a low heat flux, except at the South Pole. We investigate different models to generate the thermal anomaly in this region. We look for mechanisms that could have locally enhanced tidal dissipation in the ice, and/or in the silicate phase (e.g., magma chamber). Models using radiogenic species and tidal dissipation can raise the core temperature to the vicinity of 1000 K. This allows the presence of a liquid layer (whose thickness remains to be modeled) at the interface between the rocky core and an icy mantle. If at the rock-ice interface water can percolate into the rock, hot water and supersaturated steam can be produced. Hot water and hot steam are useful for producing the observed hydrothermal effects and morphology. (We note that if a moderate sized silicate magma chamber is present on Enceladus, present-day tidal dissipation would be sufficient to maintain it in the molten state.) We also discuss the link between this thermal model and the observed shape and geology. This work was carried out by JPL under contract with NASA.

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