  During the spin-up phase of a large pulsar glitch - a sudden decrease of the
rotational period of a neutron star - the angular velocity of the star may
overshoot, namely reach values greater than that observed for the new
post-glitch equilibrium. These transient phenomena are expected on the basis of
theoretical models for pulsar internal dynamics and their observation has the
potential to provide an important diagnostic for glitch modelling. We present a
simple criterion to assess the presence of an overshoot, based on the minimal
analytical model that is able to reproduce an overshooting spin-up. We employ
it to fit the data of the 2016 glitch of the Vela pulsar, obtaining estimates
of the fractional moments of inertia of the internal superfluid components
involved in the glitch, of the rise and decay timescales of the overshoot, and
of the mutual friction parameters between the superfluid components and the
normal one. We study the cases with and without strong entrainment in the
crust: in the former, we find indication of a large inner core strongly coupled
to the observable component and of a reservoir of angular momentum extending
into the core to densities below nuclear saturation, while in the latter a
large reservoir extending above nuclear saturation and a standard normal
component without inner core are suggested.
