Fine, nickel-poor Fe-Ni grains in the olivine of unequilibrated ordinary chondrites

Details Fine, nickel-poor Fe-Ni grains in the olivine of unequilibrated ordinary chondrites Fine, nickel-poor Fe-Ni grains in the olivine of unequilibrated ordinary chondrites

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982gecoa..46..929r&link_type=abstract

Geochimica et Cosmochimica Acta, vol. 46, June 1982, p. 929-939.

Computer Science

13

Chondrites, Chondrule, Meteoritic Composition, Olivine, Petrography, Iron Compounds, Iron Oxides, Nickel Compounds, Pyroxenes, Reduction (Chemistry), Meteorites, Ordinary Chondrites, Nickel, Abundance, Grains, Iron, Data, Olivine, Alloys, Inclusions, Chondrules, Unequilibrated Meteorites, St. Mary'S Meteorite, Bishunpur Meteorite, Characteristics, Observations, Features, Glasses, Metals, Formation, Reduction, Experiments, Origin, Procedure, Petrology, Photomicrographs, Composition, Samples, Meteorite, Conce

Scientific paper

Nickel-poor Fe-Ni grains smaller than 2.0 microns are common inclusions in ordinary, unequilibrated chondrites' porphyritic chondrule olivine, where the olivine grains seem to be relicts that survived chondrule formation without melting. This 'dusty' metal, whose most common occurrence is in the core of olivine grains having clear, Fe-poor rims, appears to be the product of the in situ reduction of FeO from the host olivine, with H2 or carbonaceous matter being the most likely reductants. H2 may have been implanted by solar wind or solar flare irradiation, but this requires the dissipation of nebular gas before the end of the chondrule formation process. Carbonaceous matter may have been implanted by shock. The large relict olivine grains may be nebular condensates or fragments broken from earlier chondrule generations.

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