Bright crater outflows: Possible emplacement mechanisms

Details Bright crater outflows: Possible emplacement mechanisms Bright crater outflows: Possible emplacement mechanisms

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992lpico.789...20c&link_type=abstract

In Lunar and Planetary Inst., Papers Presented to the International Colloquium on Venus p 20-21 (SEE N93-14288 04-91)

Other

Backscattering, Impact Melts, Planetary Craters, Planetary Evolution, Planetary Geology, Terrestrial Planets, Venus (Planet), Venus Surface, High Pressure, High Temperature, Rocks

Scientific paper

Lobate features with a strong backscatter are associated with 43 percent of the impact craters cataloged in Magellan's cycle 1. Their apparent thinness and great lengths are consistent with a low-viscosity material. The longest outflow yet identified is about 600 km in length and flows from the 90-km-diameter crater Addams. There is strong evidence that the outflows are largely composed of impact melt, although the mechanisms of their emplacement are not clearly understood. High temperatures and pressures of target rocks on Venus allow for more melt to be produced than on other terrestrial planets because lower shock pressures are required for melting. The percentage of impact craters with outflows increases with increasing crater diameter. The mean diameter of craters without outflows is 14.4 km, compared with 27.8 km for craters with outflows. No craters smaller than 3 km, 43 percent of craters in the 10- to 30-km-diameter range, and 90 percent in the 80- to 100-km-diameter range have associated bright outflows. More melt is produced in the more energetic impact events that produce larger craters. However, three of the four largest craters have no outflows. We present four possible mechanisms for the emplacement of bright outflows. We believe this 'shotgun' approach is justified because all four mechanisms may indeed have operated to some degree.

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