The evolution of Enceladus

Details The evolution of Enceladus The evolution of Enceladus

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...53..319s&link_type=abstract

(Saturn Conference, Tucson, AZ, May 11-15, 1982.) Icarus, vol. 53, Feb. 1983, p. 319-331.

Mathematics

Logic

94

Enceladus, Planetary Evolution, Satellite Surfaces, Structural Properties (Geology), Ammonia, Crusts, Geology, Grooves, Planetary Surfaces, Surface Properties, Tectonics, Formation, Volcanism, Theoretical Studies, Calculations, Conductivity, Eccentricity, Observations, Saturn, Satellites, Enceladus, Resurfacing, Tectonism, Interiors, Crust, Evolution, Fracturing, Eruptions, Ice, Surface, Ammonia, Convection, Thickness, Water, Thermal Properties, Melting, Tidal Effects, Heating, Geology, Features, Analysis

Scientific paper

Evidence is adduced for several episodes of geologic resurfacing and extensional tectonism spreading over much of the history of the small, icy Saturn moon Enceladus. Resurfacing was the product of fresh material eruptions that may have contained ammonia, which may also have made melting in the interior more likely. Tidal dissipation seems to be the only heating mechanism capable of melting Enceladus. For the thermal properties of pure H2O, the orbital eccentricity would have to be higher than the present value of 0.0044 by a factor of 5-7 in order to maintain a molten interior, and may have to be greater by a factor of 20 in order to cause melting in an initially frozen body. Removal of eccentricity forcing would result in rapid eccentricity damping, freezing, and the cessation of tectonic activity.

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