Effects of symmetry energy on the radius and tidal deformability of neutron stars in relativistic mean-field model

Understand

The radii and tidal deformabilities of neutron stars are investigated in the framework of relativistic mean-field (RMF) model with different density-dependent behaviors of symmetry energy.

• To study the effects of symmetry energy on the properties of neutron stars, an $\omega$ meson and $\rho$ meson coupling term is included in a popular RMF Lagrangian, i.e.
• the TM1 parameter set, which is used for the widely used supernova equation of state (EoS) table.
• The coupling constants relevant to the vector-isovector meson, $\rho$, are refitted by a fixed symmetry energy at subsaturation density and its slope at saturation density, while other coupling constants remain the same as the original ones in TM1 so as to update the supernova EoS table.