Water ice polymorphs and their significance on planetary surfaces

Details Water ice polymorphs and their significance on planetary surfaces Water ice polymorphs and their significance on planetary surfaces

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...44..511g&link_type=abstract

(IAU, American Astronautical Society, COSPAR, University of Hawaii, and NASA, Colloquium on the Satellites of Jupiter, 57th, Kai

Astronomy and Astrophysics

Astronomy

21

Astronomical Spectroscopy, Ice, Metamorphism (Geology), Meteoritic Damage, Natural Satellites, Planetary Surfaces, Polymorphism, Crystal Lattices, Infrared Spectra, Phase Transformations, Regolith, Remote Sensors, Tables (Data), Temperature Effects, Thermodynamic Equilibrium, Ultraviolet Spectra

Scientific paper

Impacts into an icy surface could produce significant amounts of high pressure forms of water ice. Due to the relatively low ambient surface temperatures on satellites in the outer solar system and the modest temperature rises accompanying the impact pressures required for water ice metamorphism, high-pressure polymorphs will be created by and may remain after large cratering events. If so, those high-pressure ices should be ubiquitous. Low-pressure cubic ice may be abundant as well. Impacts into an icy regolith may both produce high-pressure polymorphs from ice I and destroy high-pressure polymorphs already present. The result will be an (unknown) equilibrium concentration of high pressure polymorphs in the regolith. Polymorphs may be detectable and mappable by reflection spectroscopy at vacuum ultraviolet and mid-infrared wavelengths.

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