Nuclear Reactions in Stars. IV. Buildup from Carbon

Details Nuclear Reactions in Stars. IV. Buildup from Carbon Nuclear Reactions in Stars. IV. Buildup from Carbon

Dec 1959

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1959phrv..116.1505r&link_type=abstract

Physical Review, vol. 116, Issue 6, pp. 1505-1516

Physics

40

Scientific paper

Reaction leading to the formation of C, O, and Ne at temperatures T of about 108 °K, in the core of red giant stars, had been studied previously. The nuclear reactions and resulting nucleo-genesis are now studied for a gas consisting of C12, O16, and Ne20 at 6×108 to 10×108 °K and densities around 104 g/cc. The basic reaction rates are calculated and a set of simultaneous differential equations for various abundances as a function of time is solved numerically. The C12 is destroyed by compound nucleus formation from C+C collisions in about 105 and 1 years, respectively, at 6×108 and 8.5×108 °K. The net result is the production of some additional amounts of O16 and Ne20; appreciable amounts of Na23 and the three stable magnesium isotopes (mainly Mg24) and decreasing amounts of Al27, Si, etc. The ratio of Na23 to Mg24 produced is almost 1/2 , appreciably larger than the "cosmic" ratio. During the carbon burning, protons and alphas are released. At temperatures below 7×108 °K, neutrons are produced very copiously through the sequence C12(p, γ)N13 N13-->C13 C13(α, n)O16. If small amounts of metals in the Fe-region (up to about one metal nucleus per 1000 C12 nuclei) were present originally, each metal nucleus will absorb about 30 neutrons. At temperatures above 8×108 °K, N13 is photodisintegrated and the neutron production is appreciably less.

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