Planetary phase equilibria: application to formation of Earth,Venus and Mercury

Calculations of phase equilibria in a solar mixture with variable hydrogen abundance show that the major element chemical composition of Earth and Venus can be simply explained by their formation in equilibrium at 800 and 1000 K respectively at a pressure of 1 × 10^?3 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 1 × 10^?3 atm show that nearly 96% of the silicates and 81% of metal must have been lost from the region of proto-Mercury.