The conductive propagation of nuclear flames. I - Degenerate C + O and O + NE + MG white dwarfs

Details The conductive propagation of nuclear flames. I - Degenerate C + O and O + NE + MG white dwarfs The conductive propagation of nuclear flames. I - Degenerate C + O and O + NE + MG white dwarfs

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...396..649t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 396, no. 2, Sept. 10, 1992, p. 649-667. Research supported by California Sp

Statistics

Computation

153

Degenerate Matter, Neutron Stars, Nuclear Fusion, Radiation Transport, Stellar Interiors, White Dwarf Stars, Computational Grids, Conductive Heat Transfer, Fractals, Gravitational Collapse, Reaction Kinetics, Supernovae

Scientific paper

The paper determines the physical properties - speed, width, and density structure - of conductive burning fronts in degenerate carbon-oxygen (C + O) and oxygen-neon-magnesium (O + Ne + Mg) compositions for a grid of initial densities and compositions. The dependence of the physical properties of the flame on the assumed values of nuclear reaction rates, the nuclear reaction network employed, the thermal conductivity, and the choice of coordinate system are investigated. The occurrence of accretion-induced collapse of a white dwarf is found to be critically dependent on the velocity of the nuclear conductive burning front and the growth rate of hydrodynamic instabilities. Treating the expanding area of the turbulent burning region as a fractal whose tile size is identical to the minimum unstable Rayleigh-Taylor wavelength, it is found, for all reasonable values of the fractal dimension, that for initial C + O or O + Ne + Mg densities above about 9 x 10 exp 9 g/cu cm the white dwarf should collapse to a neutron star.

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