Crustal properties of a neutron star within an effective relativistic mean-field model

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