Near-infrared reflectance spectra from bulk samples of the two SNC meteorites Zagami and Nakhla

Details Near-infrared reflectance spectra from bulk samples of the two SNC meteorites Zagami and Nakhla Near-infrared reflectance spectra from bulk samples of the two SNC meteorites Zagami and Nakhla

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999m%26ps...34..417s&link_type=abstract

Meteoritics & Planetary Science, vol. 34, no. 3, pp. 417-424 (1999).

Mathematics

Logic

13

Scientific paper

Zagami and Nakhla are achondrites and belong to the SNC meteorite group. It is generally accepted that Mars is their putative parent body. Mineralogical and chemical analyses have revealed that the major mineral phases of these two meteorites are pyroxenes, olivine, maskelynite, and plagioclase. In this work near-infrared biconical reflectance measurements were performed on sawed surfaces of chips from Zagami and Nakhla. Spectra obtained with an analytical spot diameter in the order of the mineral grain size reflect the heterogeneous distribution of different mineral phases. The characteristic absorption bands of the pyroxenes are numerically evaluated in terms of the modified Gaussian model (MGM). Spectra with overlapping absorption features are resolved into the basic absorption bands. From these results it can be estimated what kind of clinopyroxenes belongs to the investigated mineral assemblages. As a result the major clinopyroxene phase in Nakhla is calcium-rich augite, whereas in Zagami both calcium-rich and calcium-poor pyroxenes are present. By means of such a procedure laboratory spectra of minerals become more informative and may help in discussing Martian remote sensing data in the near-infrared region.

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