Mathematics – Logic
Scientific paper
Apr 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988gecoa..52..889b&link_type=abstract
Geochimica et Cosmochimica Acta (ISSN 0016-7037), vol. 52, April 1988, p. 889-900. Research supported by McCrone Associates, Inc
Mathematics
Logic
42
Carbonaceous Chondrites, Interplanetary Dust, Particle Size Distribution, Upper Atmosphere, Chemical Composition, Electron Microscopy, Halley'S Comet, Olivine, Pyroxenes, Interplanetary Dust, Chondritic Material, Samples, Extraterrestrial, Laboratory Studies, Composition, Mineralogy, Petrography, Aem, Electron Microscopy, Analysis, Abundance, Description, Comparisons, Procedure, Photomicrographs, Tem, Silicate, Particles, Pyroxene, Olivine, Smectite, Serpentine
Scientific paper
Chondritic interplanetary dust particles (IDPs) are heterogeneous aggregates of predominantly submicron mineral grains and carbonaceous material, whose bulk compositions agree within a factor of two with type CI/CM carbonaceous chondrites. The mineralogy and petrography of 25 such particles were studied by analytical electron microscopic examination of ultramicrotomed thin sections (500-1000 A thick). Four classes of chondritic IDPs were recognized, referred to as pyroxene, olivine, smectite, and serpentine, and their relative abundances were 9:4:10:2, respectively. Quantitative thin-film analyses indicate that pyroxene particles most closely resemble material emitted from comet Halley. Smectite particles may have formed from pyroxene particles by aqueous alteration of glass and enstatite crystals. Serpentine particles are the only class that are similar to the matrices of carbonaceous chondrites, but these are the least abundant chondritic IDPs. Collectively, chondritic particles are a mineralogically diverse group of extraterrestrial materials.
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