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Many of the currently available equations of state for core-collapsesupernova simulations give large neutron star radii and do not provide largeenough neutron star masses, both of which are inconsistent with some recentneutron star observations. In addition, one of the critical uncertainties inthe nucleon-nucleon interaction, the nuclear symmetry energy, is not fullyexplored by the currently available equations of state. In this article, weconstruct two new equations of state which match recent neutron starobservations and provide more flexibility in studying the dependence on nuclearmatter properties. The equations of state are also provided in tabular form,covering a wide range in density, temperature and asymmetry, suitable forastrophysical simulations. These new equations of state are implemented intoour spherically symmetric core-collapse supernova model, which is based ongeneral relativistic radiation hydrodynamics with three-flavor Boltzmannneutrino transport. The results are compared with commonly used equations ofstate in supernova simulations of 15 and 40 solar mass progenitors. We do notfind any simple correlations between individual nuclear matter properties atsaturation and the outcome of these simulations. However, the new equations ofstate lead to the most compact neutron stars among the relativistic mean-fieldmodels which we considered. The new models also obey the previously observedcorrelation between the time to black hole formation and the maximum mass of ans=4 neutron star.

Core-collapse supernova equations of state based on neutron star observations