Computer Science
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994metic..29..461d&link_type=abstract
Meteoritics (ISSN 0026-1114), vol. 29, no. 4, p. 461
Computer Science
19
Chemical Composition, Mars (Planet), Meteoritic Composition, Mineralogy, Pyroxenes, Chassignites, Nakhlites, Scanning Electron Microscopy, Trace Elements
Scientific paper
The orthopyroxenite ALH 84001 was recently reclassified by Mittlefehldt as a martian meteorite. We analyzed several aliquots from a total of 1.7 g of split 40 for major and trace elements. Mineral compositions were determined by Scanning Electron Microscopy-Energy Dispersive Spectroscopy (SEM-EDS) analysis on thin section ALH 84001,89, which does not come from the same split as our bulk sample. Nevertheless, the compositions found are practically identical to those reported by Mittlefehldt, D. W. (1994), showing that ALH 84001 is a rather homogeneous rock with regard to the composition of the minerals, although their relative proportions may vary. The chemical composition confirms ALH 84001 as a martian meteorite and not as a diogenite. A typical feature of the Howardite, Eucrite and Diogenite (HED) meteorites is their low abundances in volatile, moderately volatile, and siderophile elements compared to terrestrial and martian rocks. An exception is S: HEDs contain between 1000 and 5000 ppm S. Compared to the 3900 ppm S in the diogenite Johnstown, the 108 ppm S in ALH 84001, 40 is very low, but matches the S values for the nakhlites (300 ppm) and Chassigny (120 ppm). The exposure age of 14 +/- 2 m.y. indicates also a relationship to nakhlites and Chassigny. The high abundance of Zn, which is enriched by a factor of 160 relative to Johnstown, is typical for the martian rocks.
Burghele A.
Dreibus Gerlind
Jochum Klaus Peter
Spettel Bernhard
Wanke Heinrich
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