Comparison between State-of-the-Art supernova simulations and the Notre Dame-Livermore supernova code

In recent work [1] a comparison of many spherical core-collapse supernova (CCSN) simulation codes was made for the same 20 Mʘ, solar metallicity progenitor based upon the initial model of [2]. The nuclear equation of state adopted is the SFHo from [3]. In this talk we summarize a comparison of the Notre Dame-Livermore (NDL) general-relativistic CCSN simulation code with the results presented in [1], using the same progenitor and equation of state. Our input neutrino interactions, however, differ from those adopted in the benchmark study. We find that the hydrodynamic aspects of the simulation, including shock evolution and proto-neutron star formation, agree well with the benchmark cases. Not surprisingly, however, there are differences in the emergent neutrino light curve that can be traced to differences in the fundamental neutrino physics employed. In this talk we will analyze these differences, suggesting where future improvements may be required in the supernova simulations.

[1] O’Connor et al. (2018), J. Phys. G: Nucl. Part. Phys. 45 104001

[2] Woosley & Heger (2007) Phys. Rep. 442 269–83

[3] Steiner et al. (2013) Astrophys. J. 774 17