Tidal deformability of neutron stars with realistic nuclear energy density functionals

We investigate the constraints on the mass and radius of neutron stars by considering the tidal deformability in the merge of neutron star binaries. We employ models based on the Skyrme force and density-functional theory and select models that are consistent with empirical data of finite nuclei, measured properties of nuclear matter around the saturation density, and observation of the maximum mass of neutron stars. From the selected models, we calculate the Love number k2, dimensionless tidal deformability Λ, and mass-weighted deformability ΛÌ in the binary system. We find that all the models considered in this work give ΛÌ less than 800, which is the constraint obtained from the measurement of GW170817. The results from our models show a relationship between Λ and radius (Λ∼R7.5) for a neutron star with a fixed mass of 1.4M, which is consistent with the recent statistical analyses.