  Detailed structures of the Vela pulsar (PSR B0833-45, with a period of
$89.33$ milliseconds) are predicted by adopting a recently-constructed unified
treatment of all parts of neutron stars: the outer crust, the inner crust and
the core based on modern microscopic Brueckner-Hartree-Fock calculations. To
take the pulsar mass ranging from $1.0M_{\odot}$ to $2.0M_{\odot}$, we
calculate the central density, the core/crust radii, the core/crust mass, the
core/crustal thickness, the moment of inertia, and the crustal moment of
inertia. Among them, the crustal moment of inertia could be effectively
constrained from the accumulated glitch observations, which has been a great
debate recently, known as "glitch crisis". Namely, superfluid neutrons
contained in the inner crust, which are regarded as the origin of the glitch in
the standard two-component model, could be largely entrained in the nuclei
lattices, then there may not be enough superfluid neutrons ($\sim 4/5$ less
than the previous value) to trigger the large glitches ($\Delta \nu/\nu_0 \sim
10^{-6}$) in the Vela pulsar. We then provide the first analysis of the crisis
based on the microscopic basis, by confronting the glitch observations with the
theoretical calculations for the crustal moment of inertia. We find that
despite some recent opposition to the crisis argument, the glitch crisis is
still present, which means that besides the crust superfluid neutrons, core
neutrons might be necessary for explaining the large glitches of the Vela
pulsar.
