Equation of state effects in the core collapse of a 20 M_{⊙} star
Abstract
Uncertainties in our knowledge of the properties of dense matter near and above nuclear saturation density are among the main sources of variations in multimessenger signatures predicted for corecollapse supernovae (CCSNe) and the properties of neutron stars (NSs). We construct 97 new finitetemperature equations of state (EOSs) of dense matter that obey current experimental, observational, and theoretical constraints and discuss how systematic variations in the EOS parameters affect the properties of cold nonrotating NSs and the core collapse of a 20 M_{⊙} progenitor star. The core collapse of the 20 M_{⊙} progenitor star is simulated in spherical symmetry using the generalrelativistic radiationhydrodynamics code uc(GR1D) where neutrino interactions are computed for each EOS using the uc(NuLib) library. We conclude that the effective mass of nucleons at densities above nuclear saturation density is the largest source of uncertainty in the CCSN neutrino signal and dynamics even though it plays a subdominant role in most properties of cold NS matter. Meanwhile, changes in other observables affect the properties of cold NSs, while having little effect in CCSNe. To strengthen our conclusions, we perform six octant threedimensional CCSN simulations varying the effective mass of nucleons at nuclear saturation density. We conclude that neutrino heating and, thus, the likelihood of explosion is significantly increased for EOSs where the effective mass of nucleons at nuclear saturation density is large.
 Publication:

Physical Review C
 Pub Date:
 November 2019
 DOI:
 10.1103/PhysRevC.100.055802
 arXiv:
 arXiv:1906.02009
 Bibcode:
 2019PhRvC.100e5802S
 Keywords:

 Astrophysics  High Energy Astrophysical Phenomena;
 Nuclear Theory
 EPrint:
 21 pages, 13 figures, 2 tables