The hydrodynamics of stellar collapse

Details The hydrodynamics of stellar collapse The hydrodynamics of stellar collapse

Apr 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...221..304v&link_type=abstract

Astrophysical Journal, Part 1, vol. 221, Apr. 1, 1978, p. 304-319. Research supported by the Shirley Farr Fund

Astronomy and Astrophysics

Astrophysics

70

Gravitational Collapse, Hydrodynamics, Shock Wave Propagation, Stellar Evolution, Stellar Models, Adiabatic Conditions, Neutron Stars, Shock Fronts, Stellar Mass

Scientific paper

Adiabatic (no transport of energy) evolutionary calculations are made to study the pure hydrodynamic motions of collapsing cores of massive stars. The equation of state is parameterized by an adiabatic index varying with density. The results of the evolution, in particular the densities and amplitude of the bounce, and the energy ejected from the surface by a reflected shock wave, are presented for a large number of parameters in the equation of state. Emphasis is placed in finding those parameters most favorable for mass ejection. The ejected energy depends mainly on the adiabatic index in the mantle rather than on the energy in the bounce. The evolutionary parameters scale simply with the total mass. The relevance of these calculations to transport calculations is considered. The remnant left by those models ejecting mass, for an initial 1.4-solar masses configuration, will evolve to a neutron star of mass about 1.3 solar masses.

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