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Stratigraphic correlation of the radar‐detected subsurface interface in Mare Crisium

1978; American Geophysical Union; Volume: 5; Issue: 9 Linguagem: Inglês

10.1029/gl005i009p00811

1944-8007

T. A. Maxwell, R. J. Phillips,

Astro and Planetary Science

The delineation of spectrally distinct units in Mare Crisium allows a more complete interpretation of the single subsurface interface detected by the Apollo lunar sounder experiment. This interface is approximately 1400 m below the surface in the central mare region of Crisium, and 1000 m below the surface in the eastern bench region. Based on the power of the returned signal, and the small difference in dielectric constant of returned lunar basalts, it is probable that this interface represents a buried regolith between two major basin‐filling episodes. The contact between spectral Units 1 and 2 is the most likely cause for the radar‐reflecting interface. Based on this model, the thickness of Unit 3 is 400 m in the eastern part of the mare, and that of Unit 2 is 1000 m. Estimates of the original depth/diameter relations of Pierce are consistent with excavation of an older basalt from below a depth of 1400 m.