Computer Science – Numerical Analysis
Scientific paper
Feb 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980nyasa.336..358w&link_type=abstract
In: Texas Symposium on Relativistic Astrophysics, 9th, Munich, West Germany, December 14-19, 1978, Proceedings. (A80-42502 18-90
Computer Science
Numerical Analysis
33
Gravitational Collapse, Neutrinos, Numerical Analysis, Stellar Evolution, Stellar Mass Ejection, Stellar Models, Cores, Equations Of State, Particle Motion, Stellar Temperature
Scientific paper
The results of a detailed numerical calculation of the collapse of the iron core of a 15 solar mass star at the end of its normal evolution are presented. The model discussed is derived from Wilson (1978) with changes in the equation of state, the electron capture model and a complete proper treatment of neutrino degeneracy. The effect of the new equation of state is to allow the collapse to proceed to about twice nuclear density before bounce occurs, and much higher infall velocities are realized. Attention is given to the temperature and entropy of the central zone as functions of the central density during the initial infall to velocity profiles before and after bounce and to the neutronization wave.
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