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M.L. Baird, E.J. Lentz (U. Tenn./ORNL), W.R. Hix, A. Mezzacappa (ORNL/U. Tenn.), O.E.B. Messer (ORNL), M. Liebendoerfer (U. Basel), TeraScale Supernova Initiative Collaboration
One of the key ingredients to the core collapse supernova mechanism is the physics of matter at or near nuclear density. Included in simulations as part of the Equation of State (EOS), nuclear repulsion experienced at high densities are responsible for the bounce shock, which initially causes the outer envelope of the supernova to expand, as well as determining the structure of the newly formed proto-neutron star. Recent years have seen renewed interest in this fundamental piece of supernova physics, resulting in several promising candidate EOS parameterizations. We will present the impact of these variations in the nuclear EOS using spherically symmetric, Newtonian and General Relativistic neutrino transport simulations of stellar core collapse and bounce.
This work is supported in part by SciDAC grants to the TeraScale Supernovae Initiative from the DOE Office of Science High Energy, Nuclear, and Advanced Scientific Computing Research Programs. Oak Ridge National Laboratory is managed by UT-Battelle, LLC, for U.S. Department of Energy under contract DEAC05-00OR22725
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.