  Large pulsar glitches (like the ones detected in the Vela) are though to be a
consequence of the superfluid component present in the interior of mature
neutron stars. However strong entrainment challenges this picture. We study the
impact of entrainment on the angular momentum that can be exchanged between the
normal component and the superfluid during a glitch by means of a consistent
global model. This allows to estimate the maximum angular momentum reservoir
stored into the superfluid component of the star: the essential ingredient are
newly calculated mesoscopic pinning forces that block the superfluid vorticity
in the crust of the neutron star. This method can also provide a quantitative
test for global models of rotating neutron stars, as well as for microphysical
inputs present in literature (like entrainment parameters and pinning forces).
