NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE

Journal Article · Tue Mar 20 00:00:00 EDT 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/748/1/70· OSTI ID:22016152

Hempel, M; Liebendoerfer, M ^[1]; Fischer, T ^[2]; Schaffner-Bielich, J ^[3]

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1. Departement Physik, Universitaet Basel, Klingelbergstr. 82, 4056 Basel (Switzerland)
2. GSI, Helmholtzzentrum fuer Schwerionenforschung GmbH, Planckstr. 1, 64291 Darmstadt (Germany)
3. Institut fuer Theoretische Physik, Ruprecht-Karls-Universitaet, Philosophenweg 16, 69120 Heidelberg (Germany)

We discuss three new equations of state (EOS) in core-collapse supernova simulations. The new EOS are based on the nuclear statistical equilibrium model of Hempel and Schaffner-Bielich (HS), which includes excluded volume effects and relativistic mean-field (RMF) interactions. We consider the RMF parameterizations TM1, TMA, and FSUgold. These EOS are implemented into our spherically symmetric core-collapse supernova model, which is based on general relativistic radiation hydrodynamics and three-flavor Boltzmann neutrino transport. The results obtained for the new EOS are compared with the widely used EOS of H. Shen et al. and Lattimer and Swesty. The systematic comparison shows that the model description of inhomogeneous nuclear matter is as important as the parameterization of the nuclear interactions for the supernova dynamics and the neutrino signal. Furthermore, several new aspects of nuclear physics are investigated: the HS EOS contains distributions of nuclei, including nuclear shell effects. The appearance of light nuclei, e.g., deuterium and tritium, is also explored, which can become as abundant as alphas and free protons. In addition, we investigate the black hole formation in failed core-collapse supernovae, which is mainly determined by the high-density EOS. We find that temperature effects lead to a systematically faster collapse for the non-relativistic LS EOS in comparison with the RMF EOS. We deduce a new correlation for the time until black hole formation, which allows the determination of the maximum mass of proto-neutron stars, if the neutrino signal from such a failed supernova would be measured in the future. This would give a constraint for the nuclear EOS at finite entropy, complementary to observations of cold neutron stars.

• OSTI ID: 22016152
• Journal Information: Astrophysical Journal, Vol. 748, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ABUNDANCE
BLACK HOLES
COLD NEUTRONS
COSMOLOGICAL MODELS
COSMOLOGY
DEUTERIUM
ENTROPY
EQUATIONS OF STATE
GALACTIC EVOLUTION
HYDRODYNAMICS
MEAN-FIELD THEORY
NEUTRINOS
NEUTRON STARS
NUCLEAR MATTER
NUCLEAR REACTIONS
NUCLEOSYNTHESIS
PROTONS
RELATIVISTIC RANGE
SUPERNOVAE
TRITIUM