CORE-COLLAPSE SUPERNOVA EQUATIONS OF STATE BASED ON NEUTRON STAR OBSERVATIONS

By A. Steiner, M. Hempel, Tobias Fischer. 2012

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Many of the currently available equations of state for core-collapse supernova simulations give large neutron star radii and do not provide large enough neutron star masses, both of which are inconsistent with some recent neutron star observations. In addition, one of the critical uncertainties in the nucleon–nucleon interaction, the nuclear symmetry energy, is not fully explored by the currently available equations of state. In this article, we construct two new equations of state which match recent neutron star observations and provide more flexibility in studying the dependence on nuclear matter properties. The equations of state are also provided in tabular form, covering a wide range in density, temperature, and asymmetry, suitable for astrophysical simulations. These new equations of state are implemented into our spherically symmetric core-collapse supernova model, which is based on general relativistic radiation hydrodynamics with three-flavor Boltzmann neutrino transport. The results are compared with commonly used equations of state in supernova simulations of 11.2 and 40 M☉ progenitors. We consider only equations of state which are fitted to nuclear binding energies and other experimental and observational constraints. We find that central densities at bounce are weakly correlated with L and that there is a moderate influence of the symmetry energy on the evolution of the electron fraction. The new models also obey the previously observed correlation between the time to black hole formation and the maximum mass of an s = 4 neutron star.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/b5e26778fe0b3f730b6659920e736518566ff450

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Citations in the corpus

Antinuclei in heavy-ion collisions (2018, background): “Possible solutions include deconfinement to quark matter, or alternative Y N and Y Y couplings [212, 213, 214, 215, 216, 217, 218, 219].”
A successful 3D core-collapse supernova explosion model (2018, methodology): “For this project, we used a monopole approximation for relativistic gravity following Marek et al. (2006), as described in Appendix A, and employed the SFHo equation of state (Steiner et al. 2013), which is consistent with all currently known nuclear constraints (Tews et al. 2017).”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “Stellar and nuclear matter is treated using the SFHo equation of state (EOS; Steiner et al. 2013).”
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].”
Global comparison of core-collapse supernova simulations in spherical symmetry (2018, methodology): “Below this temperature, for the present study we consider a low density EOS with only one nucleus 28Si.”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, methodology): “Bauswein et al. (2017) combined this observation with empirical relations between NS radii and the threshold mass for prompt collapse, which was previously found by means of simulations with an approximate treatment of general relativity (GR; Bauswein et al. 2013a), to tentatively rule out EOSs pred”
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, methodology): “For our survey we consider four different nuclear EOSs: the DD2 EOS (Hempel & Schaffner-Bielich 2010; Typel et al. 2010), the BHBΛf EOS (Banik et al. 2014), the LS220 EOS (Lattimer & Swesty 1991), and the SFHo EOS (Steiner et al. 2013).”
NEW HYPERON EQUATIONS OF STATE FOR SUPERNOVAE AND NEUTRON STARS IN DENSITY-DEPENDENT HADRON FIELD THEORY (2014, methodology): “The first supernova EoS table directly based on measured masses and radii of neutron stars was developed by Steiner and collaborators (Steiner et al. 2013).”
Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state (2017, methodology): “Measurements of NS masses and radii together can put strong constraints on the EoS (Read et al. 2009; Özel & Psaltis 2009; Özel et al. 2010; Steiner et al. 2010; Guillot et al. 2013; Steiner et al. 2013a,b; Özel et al. 2016).”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “Here, we demonstrate these components using as an example our non-rotating MZAMS = 10M model (M10 SFHo) with the SFHo EOS, including the many-body corrections to the neutrino-nucleon scattering cross section (Horowitz et al. 2017).”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, methodology): “We use for this extensive suite of simulations the SFHo EOS of Steiner et al. (2013).”