  We construct a two-component analytic model of the Vela pulsar which can
reproduce the fractional crustal moment of inertia, $I_{\rm crust}/I_{\rm
total} \geq 0.074$ ( where $I_{\rm crust}$ represents the moment of inertia of
the crust and $ I_{\rm total}$ is the total moment of inertia of the star) for
the mass range $M/M_\odot \geq 1.0 - 1.96$. The models are assumed to be
self-bound at the surface density $E_a = 2\times 10^{14}\rm g{cm}^{-3}$ (like,
Brecher and Caporaso \cite{Ref1}) which yields the transition density at the
core-crust boundary $E_b \geq 2.105 \times 10^{14}\rm g{cm}^{-3}$ and
pressure/energy-density ratio, $P_b/E_b \geq 0.00589$.The central density,
$E_0$, of the models ranges from 1.263 - 1.600 $\times 10^{15}\rm g{cm}^{-3}$.
The total moment of inertia, $I_{\rm total}$, and the moment of inertia of the
crust component, $ I_{\rm crust}$ lie in the range $I_{\rm 45} = $0.076 - 2.460
and 0.0056 - 0.8622 respectively (where $I_{45}=I/10^{45}\rm g{cm}^2$. The
total radii, $a$, of the models have the values from 9.252km - 11.578km and the
crustal thickness, $a_{\rm crust}$, lies in the range 0.234km - 1.551km. The
mass of the crust, $M_{\rm crust}/M_\odot$, of the models varies from 0.025 -
0.263. The pressure/energy-density ratio, $P_b/E_b$, at the core-crust boundary
and other physical parameters obtained in this study for the Vela pulsar are
compared with the corresponding parameters obtained in the literature on the
basis of various equations of state (EOSs). That few studies available in the
literature \cite{Ref2}, \cite{Ref3} which predict the fractional crustal moment
of inertia about 7\% for the Vela mass as large as 1.7$M_\odot$, the present
study has been able to reproduce the minimum fractional crustal moment of
inertia about 7.4\% and larger for all the values of the mass in the range 1.0
- 1.96$M\odot$ considered for the Vela pulsar.
