Planetary phase equilibria - Application to formation of earth, Venus and Mercury

Details Planetary phase equilibria - Application to formation of earth, Venus and Mercury Planetary phase equilibria - Application to formation of earth, Venus and Mercury

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981gecoa..45..813s&link_type=abstract

Geochimica et Cosmochimica Acta, vol. 45, June 1981, p. 813-820. Research supported by the City University Research Foundation;

Mathematics

Logic

Chemical Equilibrium, Phase Transformations, Planetary Composition, Planetary Evolution, Protoplanets, Terrestrial Planets, Abundance, Chemical Composition, Earth (Planet), Mercury (Planet), Mineralogy, Venus (Planet), Planets, Phases, Equilibrium, Formation, Earth, Venus, Mercury, Gases, Hydrogen, Abundance, Major Elements, Chemistry, Composition, Pyroxene, Pressure, Iron, Mineralogy, Silicates, Metals, Procedure, Thermochemistry, Planetesimals, Olivine, Spinel, Garnet

Scientific paper

Calculations of phase equilibria in a solar mixture with variable hydrogen abundance show that the major element chemical composition of the earth and Venus can be simply explained by their formation in equilibrium at 800 and 1000 K, respectively, at a pressure of 0.001 atm, provided that there is an iron loss from the region of proto-Venus relative to the solar nebula. The calculated mineralogical chemical compositions of the two planets are in excellent agreement with the available chemical and physical data. Phase equilibrium calculations at 1500 K and 0.001 atm show that nearly 96% of the silicates and 81% of metal must have been lost from the region of proto-Mercury.

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