Physical formulation of the problem about thermonuclear detonation of a degenerate carbon stellar core

Details Physical formulation of the problem about thermonuclear detonation of a degenerate carbon stellar core Physical formulation of the problem about thermonuclear detonation of a degenerate carbon stellar core

Apr 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977azh....54..354i&link_type=abstract

Astronomicheskii Zhurnal, vol. 54, Mar.-Apr. 1977, p. 354-366. In Russian.

Astronomy and Astrophysics

Astronomy

14

Late Stars, Main Sequence Stars, Stellar Evolution, Stellar Models, Stellar Temperature, Thermonuclear Explosions, Energy Dissipation, Hydrodynamic Equations, Reaction Kinetics, Thermonuclear Reactions

Scientific paper

A physical formulation for the problem of thermonuclear detonation of the degenerate carbon core formed in a highly evolved main-sequence star of 3.5 to 8 solar masses is presented which involves hydrodynamics, neutrino energy losses, and the kinetics of nuclear reactions and beta-decay processes. The kinetics of the main carbon-burning reaction, C-12 + C-12 yields Mg-24 + gamma-ray emission, is accurately considered in the low-temperature region (less than about 3 billion K), but the approximation of nuclear statistical equilibrium is used to describe secondary nuclear reactions at higher temperatures. The kinetics of neutronization and the accompanying neutrino energy losses are rigorously evaluated in the high-temperature region. An initial hydrostatic-equilibrium model of a degenerate carbon stellar core is obtained, its initial temperature distribution is examined, and the interdependence between detonation hydrodynamics and burning kinetics is demonstrated in a numerical solution.

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