  Observations of pulsar glitches may provide insights on the internal physics
of neutron stars and recent studies show how it is in principle possible to
constrain pulsar masses with timing observations. The reliability of these
estimates depend on the current uncertainties about the structure of neutron
stars and on our ability to model the dynamics of the superfluid neutrons in
the internal layers. We assume a simplified model for the rotational dynamics
of a neutron star and estimate an upper bound to the mass of 25 pulsars from
their largest glitch and average activity: the aim is to understand to which
extent the mass constraints are sensitive to the choice of the unknown
structural properties of neutron stars, like the extension of the superfluid
region and the equation of state. Reasonable values, within the range measured
for neutron star masses, are obtained only if the superfluid domain extends for
at least a small region inside the outer core, which is compatible with
calculations of the neutron S-wave pairing gap. Moreover, the mass constraints
stabilise when the superfluid domain extends to densities over nuclear
saturation, irrespective of the equation of state tested.
