The evolution of icy satellite interiors and surfaces

Details The evolution of icy satellite interiors and surfaces The evolution of icy satellite interiors and surfaces

May 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978icar...34..280c&link_type=abstract

Icarus, vol. 34, May 1978, p. 280-293. Research supported by the University of Arizona;

Astronomy and Astrophysics

Astronomy

37

Astronomical Models, Ice, Icy Satellites, Natural Satellites, Planetary Structure, Planetary Surfaces, Planetary Temperature, Rocks, Temperature Profiles, Jupiter, Saturn, Ganymede, Callisto, Titan, Europa, Io, Ammonia, Methane, Satellites, Formation Of, Ice, Surface, Interior

Scientific paper

The results obtained by Consolmagno (1975) with regard to the interiors of the smaller icy satellites are presented and the evolution of the surfaces of these objects in the light of the considered models is discussed. In the discussion the icy satellites are divided into two groups. Those with radii larger than 1000 km are composed primarily of high-pressure phases of ice. In the case of satellites of this group, internal heating may produce significant melting and solid-state convection may not be important. Those satellites with radii less than 1000 km will be composed primarily of ice I and rock. They will not significantly melt and internal convection is likely to be important.

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