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E. A.-N. Deneault, D. D. Clayton (Department of Physics and Astronomy, Clemson University)
We present a chemical reaction network which describes the condensation chemistry of carbon dust grains in an expanding supernova shell. Assuming an initial mixture of gaseous carbon and oxygen, carbon molecules and grains can condense due to the breakup of CO gas, which would otherwise inhibit their growth by trapping free carbon. We consider carbon to first condense into linear chains, which, at some critical length, transition into ringed isomers, which are resistant to oxidation. These isomers form the nuclei for the growth of larger carbon solids. How the abundances of grains depend on various kinetic parameters, isomerization lifetimes, and the C/O ratio is surveyed. The calculated abundances are compared with those found in primitive meteorites.
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.