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

2012/07/09 by A. W. Steiner, Andrew W. Steiner, M. Hempel +3 · 739 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astronomy #Astrophysics #Core (optical fiber) #Equation of state #Gamma-ray bursts and supernovae #Geophysics and Gravity Measurements #Gravitational collapse #Neutron star #Physics #Pulsars and Gravitational Waves Research #Star (game theory) #Stars #Stellar evolution #Supernova #Type II supernova #astro-ph.SR #nucl-th

paper · pdf · doi:10.1088/0004-637x/774/1/17

published in The Astrophysical Journal 774(1), 17 (IOP Publishing) · 10 pages, 7 figures

arxiv created 2012/07/09 · openalex publication_date 2013/08/09 · arxiv updated 2015/06/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

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.

Citations

• CONSTRAINING THE SYMMETRY PARAMETERS OF THE NUCLEAR INTERACTION

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