Other
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994metic..29q.509n&link_type=abstract
Meteoritics (ISSN 0026-1114), vol. 29, no. 4, p. 509
Other
1
Meteoritic Composition, Phase Transformations, Silicates, Xenon Isotopes, Abundance, Chemical Analysis, Cosmology, Temperature Effects
Scientific paper
Trapped noble gas components in meteorites will give constraints on their formation in the early solar system. Xenon isotopic composition similar to U-Xe or primitive Xe has recently been observed in the Tatahouine diogenite and the Lodran. The presence of U-Xe was also suggested in a silicate phase of the Brenham pallasite. Xenon isotopic ratios for six silicate samples designated as B1 to B6 are plotted in a three-isotope plot, Xe-130/Xe-132 vs. Xe-136/Xe-132. The samples were taken from the different fragments corresponding to different depths from the surface of the preatmospheric body. Concentrations of cosmogenic isotopes vary by 2 orders of magnitude from surface to deep interior. Fissiogenic Kr and Xe from U-238 and Pu-244 are negligible in all the samples. The cosmogenic ones are also negligible in the B6 sample. Xenon isotopic ratios are plotted on or close to the mixing lines, atmosphere, and U-Xe or atmosphere and solar Xe. The B6 sample is on the U-atmosphere mixing line, though the Xe isotopic ratios are not identical with those of U-Xe due to atmospheric contamination. The plot can exclude AVCC-Xe and Q-Xe as a trapped Xe in the Brenham pallasite. Noble gas element relative abundances in these samples are heavily depleted in lighter noble gases relative to those of solar-type noble gases. We measured noble gases in another silicate sample taken from the Brenham pallasite to investigate the trapped noble gases in this meteorite. We can conclude that the Xe component trapped in silicate phase of the Brenham pallasite at its formation is not AVCC but U or solar type. The U-Xe is more preferable to the solar type Xe as the trapped one.
Miura Yayoi N.
Nagao Keiichi
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