Chondrules and other components in C, O, and E chondrites Similarities in their properties and origins

Details Chondrules and other components in C, O, and E chondrites Similarities in their properties and origins Chondrules and other components in C, O, and E chondrites Similarities in their properties and origins

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983lpsc...14..275s&link_type=abstract

(American Geophysical Union and NASA, Lunar and Planetary Science Conference, 14th, Houston, TX, Mar. 14-18, 1983) Journal of Ge

Physics

15

Chondrites, Chondrule, Meteoritic Composition, Mineralogy, Evolution (Development), Meteoritic Microstructures, Olivine, Photomicrography, Planetary Nebulae, Meteorites, Chondrules, Stony Meteorites, Physical Properties, Origin, Comparisons, Carbonaceous Chondrites, H3 Chondrites, Ll3 Chondrites, Cm2 Chondrites, Co3 Chondrites, Cv3 Chondrites, Mineralogy, Petrography, Formation, Mixing, Chemistry, Metal, Reduction, Solar Nebula, Matrix, Procedure, Samples, Meteorite, Catalog, Diagrams, Photomicrographs, Nic

Scientific paper

Three types of chondrules are described that are common to H3, LL3, CM2, CO3, and CV3 chondrites. Low- and high-FeO, porphyritic olivine chondrules contain olivine with Fa0.3-8 and Fa5-50 respectively, and can easily be distinguished petrographically. Poikilitic pyroxene chondrules have 1-20 vol pct olivine (Fa0.2-8) enclosed by low-Ca pyroxene (Fs0.5-7), and also occur in E chondrites. These three types formed in separate nebular regions which had dimensions and spacings such that a few percent of the chondrules that collided to form compound chondrules were of different types. Sorting of chondrule precursor material and mixing of chondrule types probably account for most variations in bulk and mineral chemistry among chondrite groups. Metallic Fe,Ni grains containing 0.1-1 percent Cr, Si, and P are present in low-FeO olivine chondrules from all type 2 and least metamorphosed type 3 chondrites. Metal compositions reflect reduction during chondrule formation in the nebula, not nebular condensation. Opaque matrices in type 3 ordinary and carbonaceous chondrites are somewhat similar in composition and mineralogy, and probably have related origins. It is concluded that chondrules in all known chondrite groups share similar nebular origins.

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