Re-evaporation of condensed matter during the formation of the solar system

Details Re-evaporation of condensed matter during the formation of the solar system Re-evaporation of condensed matter during the formation of the solar system

Nov 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978rspsa.363..283h&link_type=abstract

Royal Society (London), Proceedings, Series A - Mathematical and Physical Sciences, vol. 363, no. 1713, Nov. 1, 1978, p. 283-288

Physics

Condensed Matter

4

Chondrites, Evaporation, Liquid-Vapor Equilibrium, Meteoritic Composition, Minerals, Solar System, Abundance, Condensation, Condensed Matter Physics, Partial Pressure

Scientific paper

From the properties of matter the conclusion is derived that the mineral assemblage characteristic of most chondritic meteorites is not at all what is expected to form directly from solar matter. Rather, the major minerals of the ordinary chondrites have chemical compositions indicative of formation from a medium greatly depleted in hydrogen and somewhat deficient in oxygen relative to solar elemental abundance ratios. The re-evaporation of condensed material, after separation from a large fraction of the gaseous components of solar matter, will lead to a medium of the appropriate composition. Such re-evaporation must have occurred at a time prior to the formation of many primitive meteorites.

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