Physics
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992lpico.789..120s&link_type=abstract
In Lunar and Planetary Inst., Papers Presented to the International Colloquium on Venus p 120-121 (SEE N93-14288 04-91)
Physics
Emissivity, Impact Resistance, Impact Strength, Meteorite Craters, Microwave Emission, Microwave Scattering, Venus (Planet), Venus Surface, Backscattering, Point Impact, Reflectance, Surface Roughness, Synthetic Aperture Radar
Scientific paper
Many of the impact craters on Venus imaged by the Magellan synthetic aperture radar (SAR) have interior floors with oblique incidence angle backscatter cross sections 2 to 16 times (3 dB to 12 dB) greater than the average scattering properties of the planet's surface. Such high backscatter cross sections are indicative of a high degree of wavelength-scale surface roughness and/or a high intrinsic reflectivity of the material forming the crater floors. Fifty-three of these (radar) bright floored craters are associated with 93 percent of the parabolic-shaped radar-dark features found in the Magellan SAR and emissivity data, features that are thought to be among the youngest on the surface of Venus. It was suggested by Campbell et al. that either the bright floors of the parabolic feature parent craters are indicative of a young impact and the floor properties are modified with time to a lower backscatter cross section or that they result from some property of the surface or subsurface material at the point of impact or from the properties of the impacting object. As a continuation of earlier work we have examined all craters with diameters greater than 30 km (except 6 that were outside the available data) so both the backscatter cross section and emissivity of the crater floors could be estimated from the Magellan data.
Campbell Don B.
Devries Christopher
Stacy Nicholas John Sholto
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