Abstract

The nuclear Equation of State (EoS) is an important component in the evolution and subsequent explosion of core collapse supernovae. We make a survey of various equations of state that can be found in the literature and analyze their effect on the explosion. To simulate the supernovae, we use the general relativistic spherically-symmetric code GR1D, modified to take into account the effects of three-dimensional turbulence through a new mixing length theory approach (STIR). We show that the viability of the explosion is quite EoS dependent and that the strength of explosions correlate best with the central entropy density right after bounce and the onset of turbulent mixing in the proto-neutron star.

Highlights

  • Core-collapse supernovae have been one of the main focuses of computational astrophysics for more than 50 years

  • Given the high densities reached inside the PNS, the dynamics of supernovae can be greatly impacted by the Equation of State (EOS)

  • They were able to vary different nuclear parameters — such as the effective mass, the symmetry energy, the incompressibility and others — while keeping all the other ones fixed. This approach allowed them to observe the impact of different properties of the EOS on the explosion. Both analyses revealed that the quantity responsible for the greatest change in PNS structure is the effective mass of nuclei at saturation density m∗n

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Summary

Introduction

Core-collapse supernovae have been one of the main focuses of computational astrophysics for more than 50 years. One of the main uncertainties affecting the physics of supernovae is the Equation of State (EOS) of nuclear matter. Corecollapse supernovae generate thermodynamic conditions that can go from very low densities in the mantle (103 g cm−3) to very high densities in the core (1015 g cm−3) as well as all the values in between. To adequately describe the explosion, a detailed knowledge of the EOS of matter across all these thermodynamic regimes is required. At high densities the EOS is still poorly constrained, especially when considering finite temperature effects [1,2,3,4]

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