Neutrino transport in core collapse supernovae.

Details Neutrino transport in core collapse supernovae. Neutrino transport in core collapse supernovae.

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jcoam.109..281m&link_type=abstract

J. Comput. Appl. Math., Vol. 109, No. 1 - 2, p. 281 - 319

Mathematics

27

Supernovae: Core Collapse, Supernovae: Neutrinos, Supernovae: Shock Waves

Scientific paper

Core collapse supernovae result when the iron core of a massive star becomes unstable at the end of the star's evolution, collapses on itself, rebounds at ultra-high densities, and produces a shock wave that will ultimately be responsible for disrupting the star. As infalling core material passes through the shock, it is compressed and heated, and the core nuclei are dissociated (broken up) at the expense of thermal, pressure-producing energy behind the shock, thereby weakening it. In addition to this energy loss, energy is carried away from the shocked region by massless particles know as "neutrinos". The shock stalls, and is later thought to be revived by a "neutrino heating" mechanism. At the time the shock stalls, the core consists of an inner "neutrinosphere" radiating neutrinos and "antineutrinos" of three "flavors": "electron", "muon", and "tau" neutrinos and their antineutrinos. This inner core will ultimately radiate away its thermal energy, cool, and go on to form a neutron star or a black hole. Revival of the stalled shock above the neutrinosphere is mediated by the absorption of electron neutrinos and antineutrinos emerging from the radiating proto-neutron star. Sufficient accuracy for a definitive simulation of the supernova outcome can be obtained only via a solution of the neutrino Boltzmann transport equations and their coupling to the hydrodynamics equations governing the evolution of the core material. In this article the authors present a numerical method to solve the neutrino Boltzmann equations coupled to the core hydrodynamics. Spherical symmetry is assumed, but their methods extend to multidimensional Boltzmann transport simulations. They also present the results of comparisons of "multigroup flux-limited diffusion" (approximate) neutrino transport and Boltzmann (exact) neutrino transport in post-core bounce supernova environments, with an eye toward the quantities central to the neutrino-heating, shock-revival mechanism.

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