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Pinning of vortex lines in the inner crust of a spinning neutron star may bethe mechanism that enhances the differential rotation of the internal neutronsuperfluid, making it possible to freeze some amount of angular momentum whicheventually can be released, thus causing a pulsar glitch. We investigate thegeneral relativistic corrections to pulsar glitch amplitudes in theslow-rotation approximation, consistently with the stratified structure of thestar. We thus provide a relativistic generalization of a previous Newtonianmodel that was recently used to estimate upper bounds on the masses ofglitching pulsars. We find that the effect of general relativity on the glitchamplitudes obtained by emptying the whole angular momentum reservoir is lessthan 30\%. Moreover we show that the Newtonian upper bounds on the masses oflarge glitchers obtained from observations of their largest recorded eventdiffer by less than a few percent from those calculated within the relativisticframework. This work can also serve as a basis to construct more sophisticatedmodels of angular momentum reservoir in a relativistic context. In particular,we present two alternative scenarios for "rigid" and "slack" vortex lines, andwe generalize the Feynman-Onsager relation to the case when both entrainmentcoupling between the fluids and a strong gravitational field are present.

Effects of general relativity on glitch amplitudes and pulsar mass upper bounds