  The neutron star maximum mass and the radius are investigated within the
framework of the relativistic mean-field (RMF) model. The variation in the
radius at the canonical mass, $R_{1.4}$, using different inner crust equation
of state (EoS) with different symmetry energy slope parameter is studied. It is
found that although the NS maximum mass and the corresponding radius do not
vary much with different inner crust EoSs, the radius and the tidal
deformability at 1.4$M_{\odot}$ vary with the different choice of crust EoS and
variation of about 1-2 km is seen in the radius at the canonical mass. For
non-unified EoSs, the crust with a low symmetry energy slope parameter produces
a low NS radius at the canonical mass. The properties of maximally rotating
neutron stars are also studied. The variation in the radius of rotating star at
the canonical mass 1.4$M_{\odot}$ is also seen with the slope parameter.
Similar to the static neutron star, the radius at 1.4$M_{\odot}$ of rotating
neutron star is affected by slope parameter of the inner crust. Other important
quantities like moment of inertia, frequency, rotational kinetic energy to
gravitational energy ratio are also calculated. The variation in these
quantities with the crust slope parameter is found to be more proportional to
the mass and the radius of NS.
