New relativistic effective interaction for finite nuclei, infinite
  nuclear matter and neutron stars
  We carry out the study for finite nuclei, infinite nuclear matter and neutron
star properties with the newly developed relativistic force named as 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 element i.e. Z=120, it is noticed that considerable shell gaps
appear at neutron numbers N=172, 184 and 198, showing the magicity of 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 $\it beta-equilibrium$ which are in good agreement with
the X-ray observations by Steiner and N\"{a}ttil\"{a}. We find that the maximum
mass of the neutron star to be 2.15$M_{\odot}$ and stellar radius 11.936 km .
Moreover, the radius and tidal deformability of a {\it canonical} neutron star
mass 1.4$M_\odot$ come out to be 13.242 km and 3.910$\times$10$^{36}$ g cm$^2$
s$^2$ respectively within this parameter set.
