The Composition of Meteoritic Matter: III. Phase Equilibria, Genetic Relationships and Planet Structure

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Abstract
An attempt has been made to study the composition of meteorites on a more quantitative basis than has been attempted heretofore. In particular, investigations have been made of experimental and theoretical approaches that might lead to more rigid comparisons between terrestrial and meteoritic matter. Stress has been placed particularly upon the following studies: (a) the distribution of elements between meteoritic phases; (b) average composition as a function of metal-phase content; (c) correlation between element distribution, thermochemical data, and general thermodynamic considerations. It is demonstrated that if one assumes that the observed distributions of elements represent equilibrium distributions, then equilibrium must have been established at temperatures of the order of 3000 C. and pressures of the order of . Similarly, it is demonstrated that the conditions at which equilibrium was achieved varied from meteorite to meteorite in such a way that the greater the metal-phase content, the greater the temperature and/or the pressure. The data indicate strongly that meteorites had their origin in a planet similar to the earth in general physicochemical characteristics.

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