Computer Science
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt........39c&link_type=abstract
Thesis (PH.D.)--STATE UNIVERSITY OF NEW YORK AT STONY BROOK, 1982.Source: Dissertation Abstracts International, Volume: 43-08,
Computer Science
9
Scientific paper
The equation of state of hot dense matter and radiative transport of energy and momentum by neutrinos are discussed in the context of Type II supernovae. The equation of state is calculated in all regimes of relevance. At subnuclear densities and high entropies nuclear statistical equilibrium is invoked; thermodynamic constraints are used to derive the properties and concentration of the representative heavy nucleus. At higher densities and low entropies, appropriate to the inner unshocked core, the phase transition to nuclear matter is accomplished in a simplified fashion. Neutrino -matter coupling is calculated employing a simple "two fluid" model which preserves the characteristics of more elaborate calculations. This model connects continuously the dense diffusive regime with the thin free streaming one. Three computer simulations of collapse, core bounce, and shock propagation are presented. The first two use a somewhat different equation of state than the third. The first uses free escape of a fraction of the neutrinos determined according to optical depth, the second the two fluid approach, and the third a trapping density. Hydrodynamical techniques used are explained and evaluated.
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