Feb 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979phdt........20a&link_type=abstract
Ph.D. Thesis Cornell Univ., Ithaca, NY.
Mathematics
Convective Heat Transfer, Lunar Evolution, Magma, Permeability, Porosity, Finite Difference Theory, Lunar Surface, Mathematical Models, Melting
Scientific paper
The principles of magma migration by porous flow and convective upwelling are applied to the modeling of the thermal evolution of the moon. Radioactive heat-producing elements are concentrated in the first partial melts formed early in the moon's history. Subsequently, magma migration causes removal of heat-producing elements to the surface. Finite difference thermal modeling of the moon shows this effect to be important. Moon models which are initially hot may have a lower present-day heat flux than colder models. Two distinct melting episodes can arise due to radioactive element distribution. The first of these is responsible for the feldspathic lunar crust; the second melting episode, between 4 and 3 billion years ago, produced the mare basalts.
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