The Role of the Equation of State in the ``Prompt'' Phase of Type II Supernovae
Abstract
We examine the role of the equation of state (EOS) of hot, dense matter in the prompt phase of stellar collapse. In order to achieve this goal, we have carried out radiation hydrodynamic simulations using an adjustable EOS that is consistent with constraints placed on the EOS by neutron star observations, nuclear systematics, and laboratory experiments. Our simulations of stellar collapse show that these constraints restrict the role that the EOS can play in determining the dynamics of shock propagation. We find that certain nuclear force parameters do not substantially affect the dynamics of collapse as strongly as previously believed. In particular, we find that the shock stall radius is practically independent of the compression modulus and symmetry energy when other constraints on the EOS are satisfied. In contrast, the nuclear symmetry energies have more profound effects on the collapse via electron capture, and these effects may be detectable by means of the neutrino signature of a nearby supernova.
 Publication:

The Astrophysical Journal
 Pub Date:
 April 1994
 DOI:
 10.1086/173974
 Bibcode:
 1994ApJ...425..195S
 Keywords:

 Collapse;
 Computational Astrophysics;
 Computerized Simulation;
 Equations Of State;
 Hydrodynamics;
 Shock Wave Propagation;
 Supernovae;
 Electron Capture;
 Free Energy;
 Helmholtz Equations;
 Interstellar Matter;
 Shock Waves;
 Stellar Models;
 Astrophysics;
 DENSE MATTER;
 EQUATION OF STATE;
 SHOCK WAVES;
 STARS: NEUTRON;
 STARS: SUPERNOVAE: GENERAL