SiC particles from asymptotic giant branch stars - MG burning and the s-process

Details SiC particles from asymptotic giant branch stars - MG burning and the s-process SiC particles from asymptotic giant branch stars - MG burning and the s-process

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...392l..79b&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 392, no. 2, June 20, 1992, p. L79-L82.

Astronomy and Astrophysics

Astrophysics

33

Asymptotic Giant Branch Stars, Cosmic Dust, Meteoritic Composition, Nuclear Fusion, Silicon Carbides, Carbonaceous Chondrites, Magnesium, Silicon, Stellar Composition, Stellar Evolution

Scientific paper

The question of whether isotopically anomalous SiC particles found in meteorites originate in AGB stars is addressed. It is shown that if the peak helium shell flash temperatures of massive (6-9 solar masses) stars are about 10 percent larger than they are normally assumed to be, alpha particle reactions with the magnesium will become significant. Then the (Mg-29)(alpha, n)Si-29 reaction produces a large excess of Si-29. With a light element nuclear reaction network, the evolution of the silicon isotopic composition during AGB evolution is calculated. It is found that the experimentally determined correlation between excess Si-29 and excess Si-30 in SiC particles from carbonaceous chondrites can indeed be naturally produced in this way. It is suggested that if the large isotopically anomalous SiC particles carrying nearly pure-process krypton and xenon do indeed originate in AGB stars, those stars were massive and had peak shell flash temperatures near 450 KM.

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