  The "glitch crisis" of Vela-like pulsars has been a great debate recently. It
might challenge the standard two-component glitch model, because large
fractions of superfluid neutrons are thought to be entrained in the lattices of
the crust part, then there is not enough superfluid neutrons to trigger the
large glitches in Vela-like pulsars. But the amount of entrainment which could
effectively constrain the fractional moment of inertia of a pulsar, is very
uncertain. In order to examine the importance of this parameter on the inner
structures of neutron stars, we relax the "glitch crisis" argument, employ a
set of most developed equations of state derived within microscopic many-body
approaches that could fulfill the recent 2-solar-mass constraint, and evaluate
their predictions for the fractional moment of inertia with two extremes of
crustal entrainment. We find a final determination of the amount of entrainment
could be closely related to the type of neutron star. If a large enough
fraction of neutrons are entrained, a Vela-like pulsar could not be a hybrid
star, namely no free quarks would be present in its core. In addition, we use
the Vela data to narrow the parameter space of hyperon-meson couplings in the
popular phenomenological relativistic mean field model.
