Infrared and radar signatures of lunar craters - Implications about crater evolutionGeological models accounting for the strongly crater size-dependent IR and radar signatures of lunar crater floors are examined. The simplest model involves the formation and subsequent 'gardening' of an impact melt layer on the crater floor, but while adequate in accounting for the gradual fading of IR temperatures and echo strengths in craters larger than 30 km in diameter, it is inadequate for smaller ones. It is concluded that quantitative models of the evolution of rock populations in regoliths and of the interaction of microwaves with regoliths are needed in order to understand crater evolutionary processes.
Document ID
19810041820
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Thompson, T. W. (Planetary Science Inst. Pasadena, CA, United States)
Cutts, J. A. (Science Applications, Inc. Planetary Science Institute, Pasadena, Calif., United States)
Shorthill, R. W. (Utah, University Salt Lake City, Utah, United States)
Zisk, S. H. (Haystack Observatory Westford, Mass., United States)