Neutrino Trapping During Gravitational Collapse of Stars
Aug, 197767 pages
Published in:
- Astrophys.J. 218 (1977) 815
DOI:
Report number:
- EFI-77-38-CHICAGO
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Abstract: (ADS)
Hydrodynamic calculations beginning from an 8-solar-mass helium-burning stellar evolutionary model are performed to investigate the initial stage of gravitational collapse of a stellar core through initial neutronization and up to core bounce. Weak-interaction processes are treated individually by reaction network techniques, neutrino transport is regarded as multigroup flux-limited diffusion, and scattering of neutrinos by electrons is considered to be 'nonconservative'. The physics of the problem is reviewed, emphasizing nuclear partition functions and important uncertainties. Some numerical results are presented which illustrate the temporal behavior of the radii of individual mass zones until core bounce, which give an overview of the collapse, and which indicate the structure of one model near core bounce. The dynamical and compositional structures of this model are discussed along with the neutrino opacity and scattering depth, the neutrino luminosity, thermalization of the neutrinos, neutrino degeneracy, and the neutronization region. It is suggested that the ultimate resolution of the question of how supernovae explode may be related to the behavior of the reflected shock at core bounce.- ASTROPHYSICS
- GRAVITATION
- N: MATTER
- NEUTRINO: EMISSION
- EMISSION: NEUTRINO
- FIELD THEORETICAL MODEL: WEINBERG
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