Chemistry, Petrology, and Noble Gases of Lunar Highland Meteorite QUE 93069

Details Chemistry, Petrology, and Noble Gases of Lunar Highland Meteorite QUE 93069 Chemistry, Petrology, and Noble Gases of Lunar Highland Meteorite QUE 93069

Sep 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995metic..30q.581s&link_type=abstract

Meteoritics, vol. 30, no. 5, page 581

Other

7

Gases, Noble, Kreep, Meteorites, Allan Hills 81005, Lunar, Macalpine Hills 88104, Queen Alexandra Range 93069, Yamato Mountains 793274, Rare Earth Elements, Regolith Breccia Siderophile Elements, Veins, Glass

Scientific paper

Several pieces of QUE93069.6 of together 0.764 g were obtained for our investigations. 43 mg were used for rare gas analysis, all other material was homogenized for analyses by INAA, XRF, and SSMS techniques (Table 1). Available for investigation was also thin section, QUE93069.33. Petrology: Our PTS shows a fragmental breccia, as described by [1]. Fine, irregular metal particles are dispersed in matrix and clasts. Glass is present as colorless spherules and fragments, and in two 20 - 200 micron wide veins cross-cutting the whole section. These glass veins are full of bubbles and the main element composition is virtually identical to that of the bulk meteorite. Chemistry: The bulk chemistry of QUE93069.6 is similar to that of the feldspar-rich lunar highland meteorite MAC88104 [1]. However, QUE93069 is the first lunar highland meteorite with a higher Ir concentration of 14.6 ppb corresponding to 3 % of a meteoritic component. The chondritic Ni/Ir and Ir/Au ratios indicate also a meteoritic origin for Ni and Au. The non-chondritic Ni/Co ratio of 15 reflects an indigenous Co concentration of 7 ppm, fitting well into the plot Co versus MgO+FeO for pristine highland rocks [2]. Equal bulk Fe contents in QUE93069 and MAC88104 imply the same portions of mafic phases. However, after correction for Fe in the meteoritic component, only 83 % of the total Fe is indigenous. This results also in a lower portion of the mafic phases which explain the about 15 % lower abundances of Sc, Cr, and Mn in QUE93069 compared to MAC88104. Except Eu all incompatible elements have a 25 % higher concentrations than in MAC88104, which can be explained by an admixture of KREEP. A typical KREEP pattern for these elements was obtained by subtracting the REE concentration of MAC88104 from those of QUE93069. Because of the high negative Eu-anomaly in KREEP, no Eu-enrichment is seen in an admixture of about 25 % KREEP to QUE93069 (Fig. 1). Noble gases: Among all lunar meteorites QUE93069 has the highest concentration of trapped solar noble gases (e.g. 4He = 6.2.10(^-3_cm(^3)STP/g) and is thus more mature than the other lunar meteorites. Also the 40Ar/36Ar = 1.90 is characteristic for lunar regolith material. The concentrations of cosmogenic noble gas nuclides is similar to that of ALH81005, MAC88104 or Y793274 [3]. The residence time within the lunar regolith is therefore several 100 Ma. References: [1] Lindstrom M. M. et al. (1995) LPS XXVI, 849-850. [2] Wanke H. et al. (1979) Proc. LPSC 10th, 611-626. [3] Eugster O. et al. (1991) GCA, 55, 3139-3148.

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