General relativistic hydrodynamics and the adiabatic collapse of stellar cores

Details General relativistic hydrodynamics and the adiabatic collapse of stellar cores General relativistic hydrodynamics and the adiabatic collapse of stellar cores

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...232..558v&link_type=abstract

Astrophysical Journal, Part 1, vol. 232, Sept. 1, 1979, p. 558-571.

Astronomy and Astrophysics

Astrophysics

72

Gravitational Collapse, Relativity, Stellar Cores, Stellar Structure, Supernovae, Adiabatic Conditions, Density Distribution, Equations Of Motion, Equations Of State, Stellar Models

Scientific paper

The collapse and supernova explosion, via the core-bounce-reflection-shock mechanism, of a spherically symmetric iron core of a massive star is studied using the full general theory of relativity (GR). The neglect of GR in some recent collapse calculations is not justified, even though the GR 'corrections' appear small. Bounces at low density (central density approximately 10 to the 13 g/cu cm), which are found in these Newtonian models, are close to critical in GR, and may not occur. With the new equation of state of Lamb, Lattimer, Pethick, and Ravenhall (1978) collapse simulations will not show a bounce until nuclear density is exceeded. The results of collapse models which bounce at neutron star densities are presented. Large explosion energies - up to 6 x 10 to the 51st ergs - are found if the bounce is near critical; the GR 'effective softening' of the equation of state then leads to the large rebound amplitude necessary for energetic explosions by the hydrodynamic mechanism. The mass division between neutron-star and black-hole formation is considered. The difference equations used for the GR hydrodynamics are presented.

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