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M. Liebendoerfer (Oak Ridge National Laboratory/University of Tennessee, Knoxville), O. E. B. Messer (ORNL/UTK), A. Mezzacappa (ORNL), W. R. Hix (ORNL/UTK), S. W. Bruenn (Florida Atlantic University), F.-K. Thielemann (University of Basel)
General relativistic multi group and multi flavor Boltzmann neutrino transport in spherical symmetry has become available - a new level of sophistication in the modeling of core collapse supernovae.We present postbounce simulations for five type II progenitors with 13-40 solar masses. Core collapse and bounce proceed in a quantitatively similar way, culminating in a rather uniform neutrino burst. At 100ms after bounce the shock stalls ~150km radius in all our models. As the outer layers of the progenitors, where the density profiles are more different, fall into the protoneutron star, the neutrino luminosities reflect the individual mass accretion rates. Based on standard input physics, and without considering convection, high infall velocities prevent significant heating for a neutrino-driven supernova in general relativity. We acknowledge funding by the NSF under contract AST-9877130, the Oak Ridge National Laboratory, managed by UT-Batelle, LLC, for the U.S. Department of Energy under contract DE-AC05-00OR22725,the Joint Institute for Heavy Ion Research, the Swiss National Science Foundation under contract 20-61822.00, NASA under contract NAG5-8405, a DoE HENP PECASE Award, and the DoE HENP SciDAC Program. Our Simulations have been carried out on the NERSC Cray SV-1.
The author(s) of this abstract have provided an email address for comments about the abstract: liebend@mail.phy.ornl.gov
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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.