Compaction and internal structure of Mimas

Details Compaction and internal structure of Mimas Compaction and internal structure of Mimas

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990icar...84..215e&link_type=abstract

Icarus (ISSN 0019-1035), vol. 84, March 1990, p. 215-225.

Statistics

Computation

24

Icy Satellites, Mimas, Planetary Structure, Satellite Surfaces, Computational Astrophysics, Rocks, Spaceborne Astronomy, Saturn, Satellites, Mimas, Thermal Properties, Porosity, Evolution, Calculations, Distribution, Temperture, Models, Compaction, Water Ice, Density, Formation, Origin, Interior, Differentiation, Rheology, Moment Of Inertia, Regolith, Thickness

Scientific paper

A two-phase flow method developed for partially molten rock is presently used, in conjunction with constitutive equations taken from hot isostatic pressing and porous materials' sintering, to investigate the coupled thermal and porosity evolution of the icy Saturnian moon, Mimas. It is assumed that the fluiddynamic behavior of ice-rock mixtures is dominated by pure-ice rheology. The calculations show that, if the ambient temperature of formation is below 120 K and surface porosity is greater than 25 percent, the distribution of porosity determined by plastic yielding can explain the value of the dimensionless moment of inertia.

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