The delayed-detonation model of Type IA supernovae. 2: The detonation phase

Details The delayed-detonation model of Type IA supernovae. 2: The detonation phase The delayed-detonation model of Type IA supernovae. 2: The detonation phase

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...427..330a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 427, no. 1, p. 330-341

Astronomy and Astrophysics

Astrophysics

57

Hydrodynamics, Mathematical Models, Nuclear Fusion, Nuclear Reactions, Stellar Mass, Supernovae, Algorithms, Luminosity, Radioactive Decay, Space Density, Statistical Distributions

Scientific paper

The investigation, by use of two-dimensional numerical hydrodynamics simulations, of the 'delayed detonation' mechanism of Khokhlov for the explosion of Type Ia supernovae is continued. Previously we found that the deflagration is insufficient to unbind the star. Expansion shuts off the flame; much of this small production of iron group nuclei occurs at lower densities, which reduces the electron-capture problem. Because the degenerate star has an adiabatic exponent only slightly above 4/3, the energy released by deflagration drives a pulsation of large amplitude. During the first expansion phase, adiabatic cooling shuts off the burning, and a Rayleigh-Taylor instability then gives mixing of high-entropy ashes with low-entropy fuel. During the first contraction phase, compressional heating reignites the material. The burning was allowed to develop into a detonation in these nonspherical models. The detonation grows toward spherical symmetry at late times. At these densities (rho approx. 107 to 108 g cm-3), either Ni-56 or nuclei of the Si-Ca group are the dominant products of the burning. The bulk yields are sensitive to the density of the star when the transition to detonation occurs. The relevance of the abundances, velocities, mixing, and total energy release to the theory and interpretation of Type Ia supernovae is discussed.

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