Viscosity of high-pressure ice VI and evolution and dynamics of Ganymede

Details Viscosity of high-pressure ice VI and evolution and dynamics of Ganymede Viscosity of high-pressure ice VI and evolution and dynamics of Ganymede

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981natur.292..225p&link_type=abstract

Nature, vol. 292, July 16, 1981, p. 225-227. Centre National de la Recherche Scientifique

Physics

21

Ganymede, Planetary Evolution, Planetary Structure, Pressure Ice, Viscosity, Convection, Flow Visualization, High Pressure, Ice Formation, Melting Points, Phase Diagrams, Pressure Gradients, Room Temperature, Shear Stress, Jupiter, Satellites, Ganymede, Ice, Viscosity, Pressure, Evolution, Dynamics, Models, Accretion, Silicon, Convection, Data, Experiments, Procedure, Phases

Scientific paper

Parmentier and Head (1979) have shown the possible relation between the viscosity value of high-pressure ices near the melting point on the evolution of the Jovian satellite Ganymede. In the considered investigation measurements have been conducted of the viscosity of high-pressure ice VI at room temperature and pressures of 1.1-1.2 GPa in a sapphire anvil cell. Fine particles were used to visualize the flow of ice down the radial pressure gradient. On the basis of the obtained results, it is concluded that the viscosity of ice VI in most of its domain of existence and within 20 C of its melting point, is lower than 10 to the 17th P, and may be even lower than 10 to the 14th P. This implies that, under conditions of homogeneous accretion for Ganymede, subsolidus convection was possible in the ice VI and most of the planet could have remained undifferentiated.

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