Computer simulations of stellar collapse and shock wave propagation

Details Computer simulations of stellar collapse and shock wave propagation Computer simulations of stellar collapse and shock wave propagation

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...103..147h&link_type=abstract

Astronomy and Astrophysics, vol. 103, no. 1, Nov. 1981, p. 147-153.

Astronomy and Astrophysics

Astrophysics

23

Computerized Simulation, Gravitational Collapse, Shock Wave Propagation, Stellar Evolution, Supernovae, Astronomical Models, Neutrinos, Neutron Stars

Scientific paper

Using recent progress in deriving realistic equations of state of matter at high densities and temperatures, the gravitational collapse of cores of massive stars through core-bounce at neutron star densities is calculated. In particular, the sensitivity of the results is analyzed with respect to details of the equation of state, neutrino emissivities in the shock region, and properties of the hydrocode. In none of the cases considered is the core-bounce followed by an explosion of the stellar mantle. Although a shock forms in every case, it is never strong enough to accelerate matter beyond the escape velocity. The result is found to be independent of both the details of the equation of state and the assumptions about neutrino losses from the shocked matter.

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