The accretion phase of core collapse supernovae

Journal Article · Wed May 21 04:00:00 EDT 2008 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.2943585· OSTI ID:21143479

Fischer, T; Liebendoerfer, M; Thielemann, K -F ^[1]; Goegelein, P ^[2]; Mezzacappa, A ^[3]

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1. Departement Physik, Universitaet Basel, CH-4056 Basel (Switzerland)
2. Institut fuer Theo. Phys., Universitaet Tuebingen, D-72076 Tuebingen (Germany)
3. Physics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831 (United States)

We present data from recent core collapse simulations, using spherically symmetric general relativistic radiation hydrodynamics featuring a three-flavor neutrino Boltzmann transport solver and an equation of state (eos) for hot and dense nuclear matter. A nuclear reaction network has recently been implemented, which allows us to investigate explosion models into the neutrino wind phase several seconds after core bounce. In the absence of an earlier explosion, the continuous accretion of outer layers of the progenitor star lead eventually to the collapse of the protoneutron star (PNS) at the very center and the formation of a black hole.

• OSTI ID: 21143479
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 1016; ISSN APCPCS; ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
BLACK HOLES
BOLTZMANN EQUATION
COMPUTERIZED SIMULATION
EQUATIONS OF STATE
FLAVOR MODEL
HYDRODYNAMICS
NEUTRINOS
NUCLEAR MATTER
NUCLEAR REACTIONS
RELATIVISTIC RANGE
SUPERNOVA REMNANTS