Collapse of degenerate iron stellar cores and the model of a supernova

Hydrodynamics equations have been used to investigate the collapse of cold iron star nucleus, the shell of which stores thermonuclear fuel. A complete system of spherically symmetric equations on hydrodynamics is solved using a computer. A hydrostatic equilibrium configuration with the mass of iron nucleus M approximately 1 Msub(S) (Msub(S)-solar mass) on the surface of which there is a carbon layer with M approximately 0.22 Msub(S) has been taken for the initial model. The profiles of physical values in different moments of nucleus collapse are presented. Depending on the temperature of matter of the envelope before the beginning of the hydrodynamic collapse a compact remnant similar to a neutron star or to a white dwarf is obtained. It is shown that in the thermonuclear Supernova model the maximum energy of the thrown-off shell resulting from a thermonuclear explosion is (5-7)x1049 erg