Implications of convection in the Moon and the terrestrial planets

Details Implications of convection in the Moon and the terrestrial planets Implications of convection in the Moon and the terrestrial planets

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pggp.rept..211t&link_type=abstract

In NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984 p 211 (SEE N85-23474 13-91)

Physics

Convection, Cosmochemistry, Lunar Core, Lunar Evolution, Planetary Geology, Terrestrial Planets, Deposition, Formations, Magma, Planetary Cores, Planetary Evolution, Structural Properties (Geology)

Scientific paper

The early evolution of the Moon and its implications for the early evolution of the Earth was studied. The study is divided into two parts: (1) studies of core formation. Cosmochemical studies strongly favor a near-homogeneous accretion of the Earth. It is shown that core segregation probably occurred within the first 10,000 years of Earth history. It is found that dissipative heating may be a viable mechanism for core segregation if sufficiently large bodies of liquid iron can form; (2) early thermal evolution of the Earth and Moon. The energy associated with the accretion of the Earth and the segregation of the core is more than sufficient to melt the entire Earth. The increase in the mantle liquidus with depth (pressure) is the dominant effect influencing heat transfer through the magma ocean. It is found that a magma ocean with a depth of 100 km would have existed as the Earth accreted. It is concluded that this magma ocean zone refined the earth resulting in the simultaneous formation of the core and the atmosphere during accretion. The resulting mantle was a well-mixed solid with a near pyrolite composition.

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