Influence of effective nucleon mass on equation of state for supernova simulations and neutron stars

We investigate the influence of effective nucleon mass on the equation of state (EOS), which is constructed for simulations of core-collapse supernovae and binary neutron-star mergers, within the relativistic mean-field (RMF) framework. The study introduces a new RMF parameter set, TM1m, which is a modification of the TM1e model with an adjusted effective mass, maintaining the saturation properties of nuclear matter. The TM1m model, with a larger effective mass ratio ($M^{\ast}/M \sim 0.8$) compared to the TM1e model ($M^{\ast}/M \sim 0.63$), is employed to construct a new EOS table, EOS5. This EOS table is designed to offer insights into the influence of effective nucleon mass on the EOS within a relativistic framework, particularly above the saturation density. The properties of cold neutron stars, calculated using the TM1m model, are compared with those of the TM1e and original TM1 models. Both the TM1m and TM1e models are found to be compatible with the latest constraints on tidal deformability and radii of neutron stars, derived from astrophysical observations.
Comment: 11 pages, 11 figures, 2 tables