Konstantin Maslov, NRNU (MEPhI) Moscow

A method of stiffening the relativistic mean-field (RMF) equation of state and its application to the description of neutron stars

It will be shown a way to make a given RMF equation of state for hadronic matter stiffer at high densities, while leaving it unchanged at lower densities. This method can be used to change the stiffness of either both isospin symmetric and asymmetric parts or only asymmetric part of the equation of state (EoS) in the RMF framework with field-dependent hadron masses and couplings. This allows to construct realistic phenomenological RMF models which are flexible enough to pass many experimental constraints.