The Accretion Phase of Core Collapse Supernovae

Conference · Thu May 01 04:00:00 EDT 2008

DOI:https://doi.org/10.1063/1.2943585· OSTI ID:958852

Fischer, T. ^[1]; Goegelein, P. ^[2]; Liebendoerfer, Matthias ^[1]; Mezzacappa, Anthony ^[3]; Thielemann, Friedrich-Karl W. ^[1]

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1. Universitat Basel, Switzerland
2. Eberhard-Karls-Universitat (University of Tubingen), Germany
3. ORNL

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.

• Research Organization: Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)
• Sponsoring Organization: USDOE
• DOE Contract Number: AC05-00OR22725
• OSTI ID: 958852
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
73 NUCLEAR PHYSICS AND RADIATION PHYSICS
BLACK HOLES
EXPLOSIONS
GALAXIES
HYDRODYNAMICS
NEUTRINOS
NUCLEAR MATTER
NUCLEAR REACTIONS
ORIGIN
RADIATIONS
STARS
SUPERNOVAE
TRANSPORT
black hole formation
explosions
supernovae