Origin of bright ring-shaped craters in radar images of Venus

Details Origin of bright ring-shaped craters in radar images of Venus Origin of bright ring-shaped craters in radar images of Venus

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981icar...48..428c&link_type=abstract

Icarus, vol. 48, Dec. 1981, p. 428-452.

Astronomy and Astrophysics

Astronomy

6

Planetary Craters, Planetary Evolution, Radar Astronomy, Radar Imagery, Venus Surface, Brightness, Computerized Simulation, Deposition, Impact Damage, Lunar Craters, Monte Carlo Method, Soil Erosion, Venus, Formation, Origin, Ringed Features, Craters, Radar Methods, Size, Imagery, Brightness, Earth-Based Observations, Deposits, Comparisons, Ejecta, Hypotheses, Erosion, Sedimentation, Weathering, Morphology, Moon, Photographs, Halos, Morphometry, Thickness, Deposition, Diameter

Scientific paper

Radar images of the Venusian surface taken at the Arecibo Observatory are examined in the context of recent study of the radar appearance of lunar craters to provide insight into the formation and evolution of Venusian features and to propose the thesis that bright ring-shaped features contain information about the rate at which Venus is being modified by depositional or erosional processes. Radar crater signatures are analyzed by crater floor and interior properties and by properties of ejecta deposits. Morphological comparisons with radar images of lunar craters are made, as well as morphometric comparisons with lunar radar crater haloes. The populations of radar bright craters on the moon and Venus is analyzed using a Monte Carlo simulation. It is concluded that the bright ring crater population does not resemble an impact crater production population.

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