Computer Science
Scientific paper
Sep 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984gecoa..48.1779r&link_type=abstract
Geochimica et Cosmochimica Acta (ISSN 0016-7037), vol. 48, Sept. 1984, p. 1779-1789.
Computer Science
37
Chondrites, Chondrule, Grain Boundaries, Meteoritic Composition, Mineralogy, Morphology, Calcium, Olivine, Pyroxenes, Solar Corona, Temperature Effects, Meteorites, Chondrites, Chondrules, Grains, Texture, Composition, Cais, Carbonaceous Chondrites, Ordinary Chondrites, Classification, Size, Drag, Samples, Meteorite, Cv3 Chondrites, H Chondrites, L Chondrites, Matrix, Ll3 Chondrites, Co3 Chondrites, Comparisons, Description, Inclusions, Thickness, Formation, Melting, Sintering, Thermal Effects, Gradients, L
Scientific paper
Coarse-grained rims composed of olivine, with or without low-Ca pyroxene, occur around all types of chondrules and compound chondrules in type 3 carbonaceous chondrites and around ordinary chondrites. The dark zoned chondrules and coarse grained rims were formed by the heating of clumps of opaque matrix material to subsolidus-subliquidus temperatures in the solar nebula. The most likely source of the heat that formed the coarse grained rims is the mechanism responsible for chondrule formation. CV chondrites may have formed in a region where the chondrule formation mechanism was less efficient, probably at greater solar distances than the ordinary chondrites. Alternatively, CV chondrules may have suffered fewer particle collisions prior to agglomeration.
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