Noble gas component organization in Apollo 14 breccia 14318 I-129 and Pu-244 regolith chronology

Details Noble gas component organization in Apollo 14 breccia 14318 I-129 and Pu-244 regolith chronology Noble gas component organization in Apollo 14 breccia 14318 I-129 and Pu-244 regolith chronology

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985lpsc...15..517s&link_type=abstract

(Lunar and Planetary Institute, NASA, American Geophysical Union, et al., Lunar and Planetary Science Conference, 15th, Houston,

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Apollo 14 Flight, Breccia, Lunar Rocks, Rare Gases, Regolith, Abundance, Chemical Composition, Iodine Isotopes, Petrology, Plutonium 244, Tables (Data), Xenon Isotopes, Moon, Samples, Lunar, Rare Gases, Apollo 14, Breccias, 14318, Iodine, Plutonium, Isotopes, Regolith, Chronology, Xenon, Comparisons, Isotopic Ratios, Experiments, Heating, Time Scale

Scientific paper

Drozd et al. (1972) have first detected the presence of Xe-129 in lunar material. Bernatowicz et al. (1979, 1980) established that this xenon component resides exclusively on grain surfaces and confirmed previous observations that it is less tightly bound than other surface components. The present investigation extends many of the observations made on the basis of a study of the 14301 to 14318, which is the only other lunar regolith breccia for which the isotopic structure of 'parentless xenon' has been accurately resolved. Actually this isotope has two parents, including Pu-244 and I-129, which are both now extinct. Attention is given to the analyzed samples, the employed analytical methods, the petrology and chemistry of the grain size separates, and stepwise heating experiments. On the basis of the obtained results, it is concluded that the I-Pu-Xe system can be used as a chronometer.

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