Neutron stars: A novel equation of state with induced surface tension

Violetta V. Sagun, Ilidio Lopes

Published 2017-09-22Version 1

A novel equation of state with the surface tension induced by particles' interaction was generalized to describe properties of the neutron stars. In such equation the interaction between particles is done via the hard-core repulsion by taking into account the proper volumes of particles. Recently, this model was successfully applied to the description of the properties of nuclear and hadron matter created in collisions of nucleons. The new approach is free of causality problems and fully thermodynamically consistent which enables us to use it to the investigation of the strongly interacting matter phase diagram properties in wide range of temperatures and baryon densities, including neutron stars. Here, we calculated the mass-radius relations for a compact star using the Tolmann-Oppenheimer-Volkov equation for two sets of parameters which satisfy the existing constraints. Accordingly, we found the parameter values that are in good agreement with the same ones obtained from the nuclear-nuclear collision data analysis. The astrophysical constraints suggest that the hard-core radius of baryons can vary between 0.425 fm and 0.476 fm.