Physics
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983lpsc...14..293r&link_type=abstract
(American Geophysical Union and NASA, Lunar and Planetary Science Conference, 14th, Houston, TX, Mar. 14-18, 1983) Journal of Ge
Physics
6
Breccia, Enstatite, Hvittis Chondrite, Impact Melts, Meteoritic Composition, Achondrites, Chondrites, Cooling, Mineralogy, Petrography, Sulfides, Meteorites, Impacts, Clasts, Hvittis, Enstatites, E Chondrites, Size, Breccias, Samples, Meteorites, El Chondrites, Aubrites, Achondrites, Composition, Stony Meteorites, Description, Parent Bodies, Formation, Comparisons, Enrichment, Sulfides, Concentration, Procedure, Melting, Petrography, Mineralogy, Photomicrographs, Thermal History
Scientific paper
The Hvittis enstatite chondrite breccia contains 5 + or - 2 vol pct dark clasts which appear to be impact melt-rocks. The largest clast (Clast A) is 2.5 cm in diameter; it has an igneous texture, no chondrules, and is depleted in metallic Fe, Ni and sulfide. Its fine grain size, low-Ni kamacite and schreibersite, and rare martensite resulted from rapid cooling. The abundance of melt-rock clasts in Hvittis suggests that the breccia resided at its parent body surface. However, the apparent absence of EL chondrites with solar wind-implanted rare gases suggests that the EL parent body was too small to develop a substantial regolith. The bulk composition of Clast A is very similar to that of average aubrites, except for a seven-fold enrichment in S, Cr, and Mn. These elements are concentrated in the sulfides. It thus is possible that the clast was derived from one of the sulfide-rich regions of the Hvittis matrix. If so, then aubrites may be genetically related to EL chondrites.
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