The induced surface tension contribution for the equation of state of neutron stars

Understand

We apply a novel equation of state (EoS) that includes the surface tension contribution induced by interparticle interaction and asymmetry between neutrons and protons, to the study of neutron star (NS) properties.

• This elaborated EoS is obtained from the virial expansion applied to multicomponent particle mixtures with hard core repulsion.
• The considered model is in full concordance with all the known properties of normal nuclear matter, provides a high-quality description of the proton flow constraints, hadron multiplicities created during the nuclear-nuclear collision experiments, and equally is consistent with astrophysical data coming from NS observations.
• The analysis suggests that the best model parameterization gives the incompressibility factor $K_{0}$, symmetry energy $J$, and symmetry energy slope $L$ at normal nuclear density equal to $200$ MeV, $30$ MeV, and $113.28-114.91$ MeV, respectively.