Physics – Nuclear Physics
Scientific paper
Feb 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982nupha.375..481b&link_type=abstract
Nuclear Physics A, Volume 375, Issue 3, p. 481-532.
Physics
Nuclear Physics
149
Scientific paper
In this paper we develop the theory of supernova explosions as produced by shock waves formed in the collapse of large stars. We are chiefly concerned with understanding the infall dynamics, shock formation, and the calculation of the shock energy in the various phases of shock formation and propagation.
In the infall of a large star, the inner core, ~0.8 Msolar, collapses homologously, while the outer regions are in quasi-free-fall. The collapse continues until the central density exceeds nuclear matter density, ρ0. Nuclear matter is extremely stiff against compression, so that when the matter reaches ρ0, pressure waves begin to travel out from the center, initially accumulating at the edge of the homologous core, the ``sonic point,'' forming a stationary shock. When sufficient pressure has been built up, the shock travels rapidly outward. Current numerical calculations are in general agreement on the conditions toward the end of the infall, giving a density distribution just preceding bounce, ρ10~ C/r37, with C ~ 3. This relation and a knowledge of the density at which the equation of state stiffens enables us to calculate most properties of the shock; in particular we give detailed prescriptions for calculating the energy initially put into the shock from the infall hydrodynamics.
As the shock moves outward from the sonic point, additional kinetic energy flows into the shock while energy is lost in dissociating nuclei. When the shock reaches the neutrino sphere, rs>~75 km, part of the shock energy is lost through neutrinos, which are emitted in a burst at that time. Existing computer calculations disagree on the amount of energy remaining in the shock. However, present indications are that with an adequate accounting of energy transport behind the shock by neutrino diffusion, the shock energy is sufficient to remove the mantle and envelope of the star, leaving a compact neutron star remnant with a gravitational mass about 1.4 Msolar.
Supported inm part by the National Science Foundation under NSF Foundation under NSF DMR 78-21069
Baym Gordon
Bethe Hans A.
Brown Gerald E.
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