A COMPARATIVE STUDY OF HYPERON EQUATIONS OF STATE IN SUPERNOVA SIMULATIONS

A comparative study of the. hyperon equations of state of Banik, Hempel and Banyopadhyay (BHB), Banik et al., and Shen et al. (denoted as HShen Lambda) for core-collapse supernova (CCSN) simulations is carried out in this work. The dynamical evolution of a protoneutron star (PNS) into a black hole is investigated in CCSN simulations in the general relativistic one-dimensional code using the BHB Lambda phi and HShen Lambda equation of state (EOS) tables and different progenitor models from Woosley & Heger. Radial profiles of the mass fractions of baryons, the density, as well as the temperature in the PNS at different moments in time, are compared for both EOS tables. The behavior of the central density of the PNS with time is demonstrated for these two Lambda hyperon EOS tables and compared with their corresponding nuclear EOS tables. It is observed that the black hole formation time is higher in the BHB Lambda phi case than in the HShen Lambda EOS case for the entire set of progenitor models adopted here, because the repulsive Lambda-Lambda interaction makes the BHB Lambda phi EOS stiffer. Neutrino emission with the Lambda hyperon EOS ceases earlier than that of its nuclear counterpart. The long-duration evolution of the shock radius and the gravitational mass of the PNS after a successful supernova explosion with enhanced neutrino heating are studied with the BHB Lambda phi EOS and s20WH07 progenitor model. The PNS is found to remain stable for 4 s and might evolve into a cold neutron star.