Effects of dispersed particulates on the rheology of water ice at planetary conditions

Details Effects of dispersed particulates on the rheology of water ice at planetary conditions Effects of dispersed particulates on the rheology of water ice at planetary conditions

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....9720883d&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 97, no. E12, p. 20,883-20,897.

Physics

57

Ice, Icy Satellites, Impurities, Rheology, Satellite Surfaces, Grain Size, Viscosity

Scientific paper

Effects of the initial grain size and the hard particulate impurities on the transient and the steady state flows of water ice I were investigated under laboratory conditions selected as appropriate for simulating those of the surfaces and interiors of large moons. The samples were molded with particulate volume fraction, phi, of 0.001 to 0.56 and particle sizes of 1 to 150 microns; deformation experiments were conducted at constant shortening rates of 4.4 x 10 exp -7 to 4.9 x 10 exp -4 per sec at pressures of 50 and 100 MPa and temperatures 77 to 223 K. The results obtained suggest that viscous drag occurs in the ice as it flows around hard particulates. Mixed-phase ice was found to be tougher than pure ice, extending the range of bulk plastic deformation vs. faulting to lower temperatures and higher strain rates. It is suggested that bulk planetary compositions of ice + rock (phi = 0.4-0.5) are roughly 2 orders of magnitude more viscous than pure ice, leading to thermal instability inside giant icy moons and possibly explaining the retention of crater topography on icy planetary surfaces.

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