Other
Scientific paper
Mar 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998m%26ps...33..313p&link_type=abstract
Meteoritics & Planetary Science, vol. 33, no. 2, pages 313-319.
Other
10
Scientific paper
We measured the noble gas isotopic abundances in lunar meteorite QUE94269 and in bulk-, glass-, and crystal-phases of lunar meteorite QUE94281. Our results confirm that QUE94269 originates from the same meteorite fall as QUE93069: both specimens yield the same signature of solar-particle-irradiation and also the cosmogenic noble gases are in agreement within their uncertainities. QUE93069/94269 was exposed to cosmic rays in the lunar regolith for about 1000 Ma and it trapped 3.5x10-4 cm3STP/g solar 36Ar, the other solar noble gases being present in proportions typical for the solar particle irradiation. The bulk material of QUE94281 contains about three times less cosmogenic and trapped noble gases than QUE93069/94269 and the lunar regolith residence time corresponds to 400 +/- 60 Ma. We show that in lunar meteorites the trapped solar 20Ne/22Ne ratio is correlated with the trapped ratio 40Ar/36Ar, that is, trapped 20Ne/22Ne may also serve as an antiquity indicator. The upper limits of the breccia compaction ages, as derived from the trapped ratio 40Ar/36Ar for QUE93069/94269 and QUE94281 are about 400 Ma and 800 Ma, respectively. We found very different regolith histories for the glass phase and the crystals separated from QUE94281. The glass phase contains much less cosmogenic and solar noble gases than the crystals, in contrast to the glasses of lunar meteorite EET87521, that were enriched in noble gases relative to the crystalline material. The QUE94281 phases yield a 40K-40Ar gas retention age of 3770 Ma, which is in the range of that for lunar mare rocks.
Eugster Otto
Polnau Ernst
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