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Differences in the equation of state (EOS) of dense matter translate intodifferences in astrophysical simulations and their multi-messenger signatures.Thus, extending the number of EOSs for astrophysical simulations allows us toprobe the effect of different aspects of the EOS in astrophysical phenomena. Inthis work, we construct the EOS of hot and dense matter based on the Akmal,Pandharipande, and Ravenhall (APR) model and thereby extend the open-sourceSROEOS code which computes EOSs of hot dense matter for Skyrme-typeparametrizations of the nuclear forces. Unlike Skrme-type models, in whichparameters of the interaction are fit to reproduce the energy density ofnuclear matter and/or properties of heavy nuclei, the EOS of APR is obtainedfrom potentials resulting from fits to nucleon-nucleon scattering andproperties of light nuclei. In addition, this EOS features a phase transitionto a neutral pion condensate at supra-nuclear densities. We show thatdifferences in the effective masses between EOSs have consequences for theproperties of nuclei in the sub-nuclear inhomogeneous phase of matter. We alsotest the new EOS of APR in spherically symmetric core-collapse of massive starswith $15M_\odot$ and $40M_\odot$, respectively. We find that the phasetransition in the EOS of APR speeds up the collapse of the star. However, thisphase transition does not generate a second shock wave or another neutrinoburst as reported for the hadron-to-quark phase transition. The reason for thisdifference is that the onset of the phase transition in the EOS of APR occursat larger densities than for the quark-to-hadron transition employed earlierwhich results in a significantly smaller softening of the high density EOS.

The APR equation of state for simulations of supernovae, neutron stars and binary mergers