Petrology and mineralogy of Type II, FeO-rich chondrules in Semarkona (LL3.0) - Origin by closed-system fractional crystallization, with evidence for supercooling

Details Petrology and mineralogy of Type II, FeO-rich chondrules in Semarkona (LL3.0) - Origin by closed-system fractional crystallization, with evidence for supercooling Petrology and mineralogy of Type II, FeO-rich chondrules in Semarkona (LL3.0) - Origin by closed-system fractional crystallization, with evidence for supercooling

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990gecoa..54.1785j&link_type=abstract

Geochimica et Cosmochimica Acta (ISSN 0016-7037), vol. 54, June 1990, p. 1785-1802.

Computer Science

75

Chondrule, Crystallization, Iron Oxides, Mineralogy, Petrology, Supercooling, Aggregates, Chromites, Igneous Rocks, Olivine, Refractory Materials, Troilite, Meteorites, Petrology, Mineralogy, Iron Oxide, Chondrules, Semarkina, Ll3 Chondrites, Chondrites, Stony Meteorites, Origin, Formation, Cooling, Fractional Crystallization, Olivine, Samples, Meteorite, Partitioning, Laboratory Studies, Compostion, Description, Temperature, Parent Material, Ordinary Chondrites, Procedure, Photomicrographs, Mesostasis, Chr

Scientific paper

The petrology of type II porphyritic olivine chondrules in Semarkona (LL3.0) has been studied in detail. Olivines in these chondrules are euhedral, Fe-rich, and are strongly zoned from cores to rims of grains in FeO (Fa10-30), Cr2O3 (0.2-0.6 wt pct), MnO (0.2-0.7 wt pct), and CaO (0.1-0.4 wt pct). Interstitial mesostasis is rich in Si, Al, and Ca and is glassy with abundant microcrystallites. Minor minerals include troilite, Fe,Ni metal, and chromite. Some olivine grains contain euhedral, fayalite-rich cores that are probably produced during initial supercooling of the chondrule melt. Rare relict grains of forsteritic olivine have compositions very similar to olivines in type IA chondrules in Semarkona and may result from disaggregation of such chondrules. Apart from these relics, all properties of type II chondrules can be described by closed-system fractional crystallization of droplets which were essentially entirely molten. Type IA chondrules may have formed from type II chondrules by loss of Fe and volatiles. Alternatively, the two chondrule types may have formed in regions of considerable diversity in the solar nebula from precursor materials with different Fe/Mg ratios.

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