Cratering history of Miranda - Implications for geologic processes

Details Cratering history of Miranda - Implications for geologic processes Cratering history of Miranda - Implications for geologic processes

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988icar...73..442p&link_type=abstract

Icarus (ISSN 0019-1035), 73, March 1988, p. 442-461.

Computer Science

19

Miranda, Planetary Craters, Planetary Geology, Planetary Surfaces, Uranus Satellites, Morphology, Northern Hemisphere, Solar System, Southern Hemisphere, Topography, Voyager 2 Spacecraft

Scientific paper

Miranda's surface is divisible into cratered terrain and coronae. The frequency of craters in the cratered terrain is variable and related to position on the satellite. The coronae are also variably cratered. Elsinore and Arden Coronae have similar crater frequencies and may have formed simultaneously. They are of intermediate age compared to the cratered terrain and to Inverness Corona, which is the youngest major terrain. Graben formation appears to have occurred both before and after the formation of the coronae reflecting periods of global expansion. Miranda's surface is, in general, the least cratered and therefore inferred to be the youngest within the Uranian system.

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