Relativistic Energy Density Functional for Astrophysical Applications

Relativistic nuclear energy density functionals (RNEDF) have become a standard framework for nuclear structure studies of ground-state properties and collective excitations over the entire nuclide chart [1]. By employing recent observational constraints on the neutron star mass, a universal RNEDF has been established that simultaneously describes the properties of finite nuclei and neutron star properties. Using the framework that includes the thermodynamic method, the RNEDF, and the quasiparticle random-phase approximation, one can explore the relationships between the properties of collective excitations in finite nuclei and the neutron star phase transition density and pressure at the inner edge separating the liquid core and the solid crust. Recently it has been shown that by employing the calculated and experimental excitation energies of giant resonances, energy weighted pygmy dipole strength, and dipole polarizability, constraints on the neutron star transition density and pressure can be obtained [2].