Lava Filled Craters and the Thermal History of the Lunar Surface

Details Lava Filled Craters and the Thermal History of the Lunar Surface Lava Filled Craters and the Thermal History of the Lunar Surface

May 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972natur.237..226b&link_type=abstract

Nature, Volume 237, Issue 5352, pp. 226-227 (1972).

Physics

1

Scientific paper

THE concept of a ``cooled crust'' is useful in studies of the thermal history of a planetary surface originating from a differentiated liquid layer of considerable thickness. The cooled crust is defined as the solid outer layer of a planetary surface increasing in temperature with depth, the lower boundary of which, at a depth Z0, is at a temperature T0 corresponding to the zero-pressure melting point of the planetary material. The physical state of the material below the boundary Z0 will depend on the thermal gradient dT/dZ and the elevation of the melting point with increasing depth due to lithostatic pressure which we indicate by dM/dZ. I assume material of basaltic composition under lunar conditions1.

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