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Pulsars are highly magnetized rotating neutron stars with a very stablerotation speed. Irrespective of their stable rotation rate, many pulsars havebeen observed with the sudden jump in the rotation rate, which is known aspulsar glitch. The glitch phenomena are considered to be an exhibit ofsuperfluidity of neutron matter inside the neutron star's crustal region. Themagnitude of such rapid change in rotation rate relative to their stablerotation frequency can quantify the moment of inertia of the crustal region tothe total moment of inertia of the star called as the fractional moment ofinertia (FMI). In this paper, we have calculated FMI for different masses ofthe star using six different representative unified equations of state (EoS)constructed under Relativistic Mean Field (RMF) framework. We have performed anevent-wise comparison of FMI obtained from data with that of theoreticallycalculated values with and without considering the entrainment effect. It isfound that larger glitches can't be explained by crustal FMI alone, evenwithout the entrainment.

Glitch Behavior of Pulsars and Contribution from Neutron Star Crust