New relativistic effective interaction for finite nuclei, infinite nuclear matter, and neutron stars

We carry out the study of finite nuclei, infinite nuclear matter, and neutron star properties with the newly developed relativistic force, the Institute of Physics Bhubaneswar-I (IOPB-I). Using this force, we calculate the binding energies, charge radii, and neutron-skin thickness for some selected nuclei. From the ground-state properties of superheavy nuclei ($Z=120$), it is noticed that considerable shell gaps appear at neutron numbers $N=172$, 184, and 198, manifesting the magicity at these numbers. The low-density behavior of the equation of state for pure neutron matter is compatible with other microscopic models. Along with the nuclear symmetry energy, its slope and curvature parameters at the saturation density are consistent with those extracted from various experimental data. We calculate the neutron star properties with the equation of state composed of nucleons and leptons in $\ensuremath{\beta}$-equilibrium, which are in good agreement with the x-ray observations by Steiner [Astrophys. J. 722, 33 (2010)] and N\"attil\"a [Astron. Astrophys. 591, A25 (2016)]. Based on the recent observation of GW170817 with a quasi-universal relation, Rezzolla et al. [Astrophys. J. Lett. 852, L25 (2018)] have set a limit for the maximum mass that can be supported against gravity by a nonrotating neutron star in the range $2.01\ifmmode\pm\else\textpm\fi{}0.04\ensuremath{\lesssim}M({M}_{\ensuremath{\bigodot}})\ensuremath{\lesssim}2.16\ifmmode\pm\else\textpm\fi{}0.03$. We find that the maximum mass of the neutron star for the IOPB-I parametrization is $2.15{M}_{\ensuremath{\bigodot}}$. The radius and tidal deformability of a canonical neutron star of mass $1.4{M}_{\ensuremath{\bigodot}}$ are 13.2 km and $3.9\ifmmode\times\else\texttimes\fi{}{10}^{36}\phantom{\rule{0.16em}{0ex}}\mathrm{g}\phantom{\rule{0.16em}{0ex}}{\mathrm{cm}}^{2}\phantom{\rule{4pt}{0ex}}{\mathrm{s}}^{2}$, respectively.