Accretional heating as the major cause of compositional differences among meteorite parent bodies, the moon, and earth

Details Accretional heating as the major cause of compositional differences among meteorite parent bodies, the moon, and earth Accretional heating as the major cause of compositional differences among meteorite parent bodies, the moon, and earth

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...43..215h&link_type=abstract

Icarus, vol. 43, Aug. 1980, p. 215-221.

Computer Science

Geochemistry, Heating, Lunar Composition, Meteoritic Composition, Planetary Composition, Protoplanets, Degassing, Deposition, Earth Planetary Structure, Planetary Evolution, Planetary Temperature, Primitive Earth Atmosphere, Planets, Accretion, Heating, Composition, Meteorites, Parent Bodies, Moon, Earth, Comparisons, Gases, Volatile Elements, Outgassing, Temperatures, Hypotheses, Models

Scientific paper

Accretional energy can be retained with sufficient efficiency in the outer layers of the moon due to the considerable amount of debris falling back into large craters. The heating of meteorite parent bodies occurs mainly after their accretion, by destructive collisions. The heating was generally not sufficient to differentiate the parent bodies completely so that iron meteorites would originate from the mantle, rather than from the core of a meteorite parent body. Assuming that the earth and moon accreted from material of similar chemical composition, it is suggested that only from the outer lunar shell is there a loss of gases and volatiles due to accretional melting. The earth melted completely and degassing was efficient for the whole mass of the earth leading to its approximately 20% higher uncompressed mean density in comparison to the moon. Because of its lower gravitational field, gases and volatiles escaped much more easily from the lunar atmosphere than from the terrestrial one, leading to the observed depletion in volatiles of the outer parts of the moon.

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