Relationships Among Isotopic Compositions of Solar-System Xenon and Krypton

Details Relationships Among Isotopic Compositions of Solar-System Xenon and Krypton Relationships Among Isotopic Compositions of Solar-System Xenon and Krypton

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27.1013p&link_type=abstract

Lunar and Planetary Science, volume 27, page 1013

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Fractionation, Grains: Interstellar, Krypton, Wind: Solar, Xenon

Scientific paper

A remarkably large number of isotopically different trapped Xe and Kr compositions have been measured in meteorite carrier phases or inferred to exist in the early solar system. For Xe these include a group here collectively termed "Q-type" Xe: Xe-Q, Xe-P1, OC (ordinary chondrite)-Xe, AVCC (average carbonaceous chondrite)-Xe, and ureilite Xe (e.g., Kenna and Novo Urei), all of which have been put forward at one time or another as candidates for "primordial" solar-system Xe. Presolar meteoritic diamonds contain a second and different suite of isotopically distinct compositions: Xe-P3, Xe-HL, and Xe-P6e ("exotic"). Another, Xe-S, is prominent in interstellar silicon carbide. Each of these is accompanied in its carrier by a corresponding Kr composition. In addition an originally inferred but now detected composition called U-Xe is a promising primordial parent for nonradiogenic terrestrial Xe; both U-Xe and its associated Kr, Kr-1, appear to be present in solar wind (SW) Xe and Kr. Such an extensive and isotopically diverse set of compositions might well be expected from nucleosynthetic theory. The possibility explored here, however, is that some of them are not truly independent, but may instead reflect fractionation or mixing of a smaller subset of primary components.

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