NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE

By M. Hempel, Tobias Fischer, Jürgen Schaffner-Bielich, M. Liebendorfer. 2011

188 citations recorded by the source corpus.

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 & 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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7b09485ecbba86d8028c18851f3181037f6d9948

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Citations in the corpus

CORE-COLLAPSE SUPERNOVA EQUATIONS OF STATE BASED ON NEUTRON STAR OBSERVATIONS (2012, methodology): “We compared the different EOS during the ironcore collapse phase, which is dominated by heavy nuclei, and confirmed already reported differences between these EOS (see, e.g., Hempel et al. 2012).”
SYSTEMATICS OF DYNAMICAL MASS EJECTION, NUCLEOSYNTHESIS, AND RADIOACTIVELY POWERED ELECTROMAGNETIC SIGNALS FROM NEUTRON-STAR MERGERS (2013, methodology): “…Bauswein et al. (2012) we extend our EoS survey by including also the models TM1, TMA, NL3, DD2, SFHO and SFHX of Hempel & Schaffner-Bielich (2010) Hempel et al. (2012) and Steiner et al. (2012), relying on the interactions described in Sugahara & Toki (1994) Toki et al. (1995), Lalazissis et al.…”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, background): “…measurements point to K = 240 MeV for symmetric nuclear matter (Shlomo et al. 2006), and because observations have recently pushed the maximum neutron star mass to at least 2M⊙ (Demorest et al. 2010), which is incompatible with this particular EoS (see Figure 1 and cp. also Hempel et al. 2012).”
Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung (2019, background): “ 1] 1 ; (5.2) with inverse temperature = 1=T and chemical potential N. Commonly used modern equations of state for supernova studies consider the strongly interacting nucleons at the mean eld level [49,70], which are based on the single-particle self energy that can be separated into scalar (S) and”
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, methodology): “We use the SFHo nuclear equation of state (EOS) (Steiner et al. 2013; Hempel et al. 2012; O’Connor & Ott 2010) everywhere.”
Unequal mass binary neutron star mergers and multimessenger signals (2016, methodology): “We continue with the same three distinct microphysical EoS (SFHo [34], DD2 [35] and NL3 [35]) used in our previous paper [22].”
Symmetry energy impact in simulations of core-collapse supernovae (2013, methodology): “ery dierent neutron matter EOSs, as will be shown below. Furthermore, the LS models lead to notable dierences in core-collapse supernova simulations compared to FSUgold as was demonstrated in refs. [28,27]. Fig. 3 shows the energy per baryon, E=N, for neutron matter at T = 0 for the same set of EOSs”
Global comparison of core-collapse supernova simulations in spherical symmetry (2018, methodology): “AGILE employs a flexible EOS module that has been implemented in [45] for the three independent variables temperature, rest-mass density and electron fraction.”
NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, methodology): “Nuclear matter description is provided by the TM1 nuclear equation of state, supplemented with electron-positron and photon contributions (Timmes & Swesty 2000; Hempel et al. 2012).”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, unknown): “…cursory study in 2D (Burrows et al. 2018) studied the EOS dependence; we deem this one of the most important topics for the future (Souza et al. 2009; Hempel et al. 2012; Couch 2013; Suwa et al. 2013; Steiner et al. 2013; da Silva Schneider et al. 2017; Nagakura et al. 2018; Schneider et al. 2019).”
NEW HYPERON EQUATIONS OF STATE FOR SUPERNOVAE AND NEUTRON STARS IN DENSITY-DEPENDENT HADRON FIELD THEORY (2014, background): “This indicates different thermal properties of the EoS, which are known to be important for neutron-star mergers (Bauswein et al. 2013; Kaplan et al. 2013) and black hole formation (Hempel et al. 2012).”
Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, methodology): “The employed microphysical EOSs are SFHO, SFHX (Steiner, Hempel & Fischer 2013), TM1 (Sugahara & Toki 1994; Hempel et al. 2012), TMA (Toki et al. 1995; Hempel et al. 2012), and DD2 (Hempel & Schaffner-Bielich 2010; Typel et al. 2010), which are all derived within the relativistic mean-field…”