Other
Scientific paper
Nov 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...44..441h&link_type=abstract
(IAU, American Astronautical Society, COSPAR, University of Hawaii, and NASA, Colloquium on the Satellites of Jupiter, 57th, Kai
Other
34
Ice, Jupiter (Planet), Planetary Composition, Planetary Evolution, Planetary Surfaces, Protoplanets, Callisto, Carbonaceous Chondrites, Chiron, Comets, Ganymede, Meteorite Craters, Phobos, Planetary Environments
Scientific paper
Observational and theoretical data converge on the conclusion that planetesimals in Jupiter's region of the solar nebula were initially composed predominantly of a mixture of roughly 39-70% H2O ice by volume, and 30-61% dark stony material resembling carbonaceous chondrites. Recent observations emphasize a division of most asteroid and satellite surfaces in this region into two distinct groups: bright icy material and dark stony material. The present model accounts for these by two main processes: an impact-induced buildup of a dark stony regolith in the absence of surface thermal disturbance, and thermal-disturbance-induced eruption of 'water magmas' that create icy surfaces. 'Thermal disturbances' include tidal and radiative effects caused by nearness of a planet. A correlation of crater density and albedo, Ganymede's dark-ray craters, and other observed phenomena (listed in the summary) appear consistent with the model discussed here.
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