Equation of State of Neutron Stars

The equation of state (EoS) of dense nuclear matter plays a central role in determining the structure and observable properties of neutron stars. In this talk, we investigate how different EoS models shape the mass–radius (M–R) relation, with particular emphasis on the lower mass limit of neutron stars. By comparing M–R curves across a range of different EoS models, which are a combination of various dense matter EoS and crust EoS models. Our goal is to identify the minimum stable neutron star mass of each EoS to provide insights into the mass boundary between neutron stars and white dwarfs.