Lava flows in Mare Imbrium - an evaluation of anomalously low earth-based radar reflectivity

Details Lava flows in Mare Imbrium - an evaluation of anomalously low earth-based radar reflectivity Lava flows in Mare Imbrium - an evaluation of anomalously low earth-based radar reflectivity

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975moon...13..395s&link_type=abstract

The Moon, vol. 13, Aug. 1975, p. 395-423. Research supported by the U.S. Geological Survey;

Mathematics

Logic

23

Lava, Lunar Maria, Lunar Radar Echoes, Reflected Waves, Frequency Distribution, Geochemistry, Ilmenite, Light Curve, Lunar Evolution, Lunar Rocks, Mapping, Signal Analysis

Scientific paper

The surface of Mare Imbrium contains some of the most distinct red-blue colorimetric boundaries and depolarized 70-cm wavelength-reflectivity variations on the near side of the moon. The weakest levels of both 3.8-cm and 70-cm reflectivity within Imbrium are confined to spectrally blue regional mare surfaces that can be recognized as stratigraphically unique flow surfaces. Frequency distributions of the 70-cm polarized and depolarized radar-return power for five mare surfaces within the basin indicate that signal absorption, and probably ilmenite content, increases generally from the beginning of the Imbrium Period to the end of the Eratosthenian Period with slight reversal between the end of the Imbrium and beginning of the Eratosthenian. TiO2 calibrated radar-reflectivity curves can be utilized for lunar-maria geochemical mapping in the same manner as the TiO2 calibrated spectral-reflectivity curves of Charette et al. (1974).

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