Isotopic composition of trace elements in presolar silicon carbide A+B grains

Details Isotopic composition of trace elements in presolar silicon carbide A+B grains Isotopic composition of trace elements in presolar silicon carbide A+B grains

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....13809s&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #13809

Physics

Condensed Matter

Materials Science

Scientific paper

Presolar SiC are classified into several types based on C, N, and Si isotopic compositions. Most are mainstream, which are generally believed to derive from low-mass asymptotic giant branch (AGB) stars. Among the less common grains, A+B grains, which comprise ˜3-4% of presolar SiC, are perhaps the least well understood. Recent measurements of trace element concentration patterns in individual grains suggest that A+B grains can be divided into at least 4 groups, and thus have multiple astrophysical sites of origin^1. We report here our Resonant Ionization Mass Spectrometry (RIMS) measurements of Zr, Mo, Ba, and Fe isotopic compositions in individual mainstream and type A+B presolar SiC. While the mainstream grains show isotopic compositions compatible with condensation around low-mass AGB stars, most A+B grains have near-solar isotopic compositions, though some show Zr, Mo, and Fe isotope patterns that have not been observed in other types of presolar SiC grains. We discuss these results in terms of possible astrophysical sites for the production of these unusual grains. This work was supported in part by the Department of Energy, BES-Materials Sciences through Contract No. W-31-109-ENG-38. ^1 Amari S., Nittler L. R., Zinner E., Lodders K., and Lewis R. S. (2001) Astrophys. J. 559, 463-483.

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