Saturn's icy satellites - Thermal and structural models

Details Saturn's icy satellites - Thermal and structural models Saturn's icy satellites - Thermal and structural models

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...54..490e&link_type=abstract

Icarus (ISSN 0019-1035), vol. 54, June 1983, p. 490-510.

Astronomy and Astrophysics

Astronomy

113

Astronomical Models, Icy Satellites, Planetary Evolution, Planetary Structure, Planetary Temperature, Saturn Satellites, Convective Heat Transfer, Cooling, Heat Sources, Silicates, Temperature Profiles, Thermal Energy, Saturn, Satellites, Icy Bodies, Thermal Properties, Structure, Models, Mimas, Tethys, Dione, Rhea, Iapetus, History, Heating, Lithosphere, Accretion, Conduction, Interiors, Convection, Comparisons, Cratering, Surface, Enceladus, Tidal Effects, Water Ice, Melting

Scientific paper

Thermal history models which assume formation as homogeneous ice-silicate mixtures are constructed for the small, icy Saturnian satellites Mimas, Tethys, Dione, Rhea, and Iapetus, including the effects of radiogenic and accretional heating, conductive and subsolidus convective heat transfer, and lithosphgeric growth. Accretional heating is not likely to have melted the water ice in the interiors of these bodies, and solid state creep of the ice-dominated material precludes melting by radiogenic heating. The four largest satellites are sufficiently large and rich in heat-producing silicates to possess a solid state convection system beneath a rigid lithosphere, irrespective of initial conditions. The model thermal histories are qualitatively consistent with the present appearances of these satellites.

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