Hydrodynamic models for explosions of rapidly rotating and collapsing supernovae with allowance for iron dissociation/recombination

Details Hydrodynamic models for explosions of rapidly rotating and collapsing supernovae with allowance for iron dissociation/recombination Hydrodynamic models for explosions of rapidly rotating and collapsing supernovae with allowance for iron dissociation/recombination

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999astl...25...93i&link_type=abstract

Astronomy Letters, Volume 25, Issue 2, February 1999, pp.93-110

Astronomy and Astrophysics

Astronomy

8

Scientific paper

We explore the topical problem of a justified allowance for the dissociation (recombination) of iron-peak nuclides into free nucleons and alpha-particles (from nucleons and alpha-particles) in terms of the two-dimensional hydrodynamic model for explosions of rotating iron cores in collapsing supernovae; this problem was stated and solved by Aksenov et al. (1997) with a rough equation of state. Because of the applicability of the nuclear statistical equilibrium (NSE) approximation, we took into account the dissociation/recombination processes by including in the universal equation of state a mixture of ideal Boltzmann gases of nuclides, Planck's radiation, and Fermi-Dirac gases of electrons and positrons with a variable chemical composition of nuclides. We present the results of a numerical solution of the problem, beginning at the instant of the explosion of a low-mass neutron star moving in an eccentric (~700 km) orbit to late stages (in ~1 s) when the front of the diverging shock wave reaches distances of ~10000 km from the center. In comparison with the previous paper by Aksenov et al. (1997), the substantiated data on the post-shock temperature and chemical composition can be considered to be of greatest interest, while the previous main conclusions about the high degree of asymmetry of the explosion with an undamped diverging shock wave have been fully confirmed with the new equation of state. We analyze the structure of the presupernova matter surrounding the exploded neutron star and invoke simple considerations about nucleosynthesis of radioactive nickel Ni-56 to determine the mass of this nickel nuclide, M_Ni = (0.04-0.08) M_solar. We took the escape velocity of the pulsar (a black hole?) v_p = 1000 km/s, which is consistent with observations and theoretical considerations, as the only important parameter of the hydrodynamic model.

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