Possible sources of H2 to H2O enrichment at evaporation of parent chondritic material

Details Possible sources of H2 to H2O enrichment at evaporation of parent chondritic material Possible sources of H2 to H2O enrichment at evaporation of parent chondritic material

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24..921m&link_type=abstract

In Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 2: G-M p 921-922 (SEE N94-16173 03-91)

Physics

Carbonaceous Chondrites, Enrichment, Evaporation, Gas Composition, Hydrogen, Meteorite Collisions, Meteoritic Composition, Olivine, Water Vapor, Carbonaceous Materials, High Temperature, Organic Compounds, Planetary Nebulae, Solar System Evolution, Water

Scientific paper

One of the results obtained from thermodynamic simulation of recondensation of the source chondritic material is that at 1500-1800 K it's possible to form iron-rich olivine by reaction between enstatite, metallic iron and water vapor in the case of (H2O)/(H2) approximately equal to 0.1. This could be reached if the gas depletion in hydrogen is 200-300 times relative to solar abundance. To get this range of depletion one needs some source material more rich in hydrogen than the carbonaceous CI material which is the richest in volatiles among chondrites. In the case of recondensation at impact heating and evaporation of colliding planetesimals composed of CI material, we obtain insufficiently high value of (H2)/(H2O) ratio. In the present paper we consider some possible source materials and physical conditions necessary to reach gas composition with (H2)/(H2O) approximately 10 at high temperature.

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