Formation of E chondrites and aubrites - A thermodynamic model

Details Formation of E chondrites and aubrites - A thermodynamic model Formation of E chondrites and aubrites - A thermodynamic model

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...43..184s&link_type=abstract

Icarus, vol. 43, Aug. 1980, p. 184-202.

Computer Science

18

Abundance, Chemical Fractionation, Chondrites, Meteoritic Composition, Thermodynamic Properties, Condensing, Metamorphism (Geology), Oxidation, Silicon, Sulfur, Trace Elements, Meteorites, E Chondrites, Aubrites, Thermodynamics, Formation, Models, Condensation, Accretion, Comparisons, Properties, Metals, Silicates, Pressure, Temperatures, Fractionation, Gases, Composition, Catalogs, Lithophile Elements, Siderophile Elements, Chalcophile Elements, Iron, Oxidation, Trace Elements, Procedure, Reduction, Oldham

Scientific paper

Condensation and accretion models for the formation of E chondrites have been examined. It is concluded that there is no simple equilibrium process which can explain all their fundamental properties. The nearest would seem to involve a complex accretion history, whereby metal and silicates which ceased to equilibrate at high temperatures and pressures (about 1200-1600 K and about 1 atm) were mixed with material which ceased to equilibrate at the same pressures but over the temperature range 600-700 K. In this way the level of reduction displayed by this class, and the fractionation of several major, minor, and trace elements, may be explained. It is difficult to escape the conclusion that two assemblages are required, even if it is assumed that these meteorites formed from a gas of nonsolar composition. However, when the lithophile element fractionation and uncertainties in the thermodynamic and cosmic abundance data are taken into account, it is possible that the gas from which this meteorite class formed had a cosmic composition prior to the beginning of condensation.

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