Unusual olivine and pyroxene composition in interplanetary dust and unequilibrated ordinary chondrites

Details Unusual olivine and pyroxene composition in interplanetary dust and unequilibrated ordinary chondrites Unusual olivine and pyroxene composition in interplanetary dust and unequilibrated ordinary chondrites

May 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989natur.339..126k&link_type=abstract

Nature (ISSN 0028-0836), vol. 339, May 11, 1989, p. 126-128.

Computer Science

70

Chondrites, Interplanetary Dust, Meteoritic Composition, Micrometeorites, Olivine, Pyroxenes, Aluminum Oxides, Chromium Oxides, Cosmochemistry, Iron Oxides, Manganese Oxides, Meteorites, Interplanetary Dust, Samples, Meteorite, Laboratory Studies, Samples, Extraterrestrial, Mineralogy, Olivine, Pyroxene, Composition, Uocs, Ordinary Chondrites, Comparisons, Chondritic Material, Grains, Iron Oxide, Manganese Oxide, Origin, Source, Condensation, Semarkona, Solar Nebula, Data, Eet Meteorites, Antarctic Meteorit

Scientific paper

The presence, in both a number of interplanetary dust particles (IDPs) and in meteorite matrices, of olivine and orthopyroxene grains, low in FeO but containing up to 5 wt pct MnO, is reported. The majority of olivines and pyroxenes in meteorites contain less than 0.5 wt pct MnO. The presence of these low-iron, manganese-enriched (LIME) olivines and pyroxenes in IDPs and meteorites may indicate a link between the origin and history of IDPs and the matrix material of primitive meteorites. The origin of the LIME silicates could be explained by condensation from a gas of solar composition. Forsterite is the first major silicate phase to condense from a solar nebula gas, and Mn, which is not stable as a metal under solar nebula conditions, would condense at about 1100 K as Mn2SiO4 in solid solution with forsterite.

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