  We use the effective relativistic mean-field (E-RMF) model to study the
crustal properties of the neutron star. The unified equations of state (EoS)
are constructed using recently developed E-RMF parameter sets, such as
FSUGarnet, IOPB-I, and G3. The outer crust composition is determined using the
atomic mass evaluation 2020 data [Chinese Physics C {\bf 45}, 030002 (2021)]
along with the available Hartree-Fock-Bogoliubov mass models [Phys. Rev. C {\bf
88}, 024308 (2013)] for neutron-rich nuclei. The structure of the inner crust
is estimated by performing the compressible liquid drop model calculations
using the same E-RMF functional as that for the uniform nuclear matter in the
liquid core. Various neutron star properties such as mass-radius ($M-R$)
relation, the moment of inertia ($I$), the fractional crustal moment of inertia
($I_{crust}/I$), mass ($M_{crust})$ and thickness ($l_{crust}$) of the crust
are calculated with three unified EoSs. The crustal properties are found to be
sensitive to the density-dependent symmetry energy and slope parameter
advocating the importance of the unified treatment of neutron star EoS. The
three unified EoSs, IOPB-I-U, FSUGarnet-U, and G3-U, reproduced the
observational data obtained with different pulsars, NICER, and glitch activity
and are found suitable for further description of the structure of the neutron
star.
