Morphology of buried craters: Lava thickness estimates by simulated flooding

Details Morphology of buried craters: Lava thickness estimates by simulated flooding Morphology of buried craters: Lava thickness estimates by simulated flooding

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984pggp.rept..107m&link_type=abstract

In NASA. Washington Rept. of Planetary Geol. Program, 1983 p 107-109 (SEE N84-23431 13-91)

Computer Science

Estimates, Lava, Morphology, Planetary Craters, Planetary Surfaces, Thickness, Floods, Geology, Tectonics, Terrain Analysis, Topography

Scientific paper

Partially and completely buried craters on planetary surfaces are used as probes to determine the thickness and extent of the overlying material as well as the composition of underlying terrain units. Rims of craters protruding through mare basalts on the Moon have been used extensively by DeHon (1977, 1979) to develop isopach maps of both the circular and irregular maria. Such estimates are possible because of Apollo topographic data and the extensive coverage by Lunar Orbiter photographs at various sun angles. On planetary surfaces without such data, however, shadow measurements can only be made by pixel listings with appropriate assumptions concerning support data. In addition, high resolution geochemical data is not available to determine whether the exposed crater rim is composed of material dissimilar from the lavas. Because of the need for lava thickness data, flooding of lunar mare and highland craters was simulated in order to determine empirical relationships between dimensions observed in orbital images and the thickness of the lava.

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