  Pulsar-like compact stars provide us a unique laboratory to explore
properties of dense matter at supra-nuclear densities. One of the models for
pulsar-like stars is that they are totally composed of "strangeons", and in
this paper we studied the pulsar glitches in a strangeon star model. Strangeon
stars would be solidified during cooling, and the solid stars would be natural
to have glitches as the result of starquakes. Based on the starquake model
established before, we proposed that when the starquake occurs, the inner
motion of the star which changes the moment of inertia and has impact on the
glitch sizes, is divided into plastic flow and elastic motion. The plastic flow
which is induced in the fractured part of the outer layer, would move
tangentially to redistribute the matter of the star and would be hard to
recover. The elastic motion, on the other hand, changes its shape and would
recover significantly. Under this scenario, we could understand the behaviors
of glitches without significant energy releasing, including the Crab and the
Vela pulsars, in an uniform model. We derive the recovery coefficient as a
function of glitch size, as well as the time interval between two successive
glitches as the function of the released stress. Our results show consistency
with observational data under reasonable ranges of parameters. The implications
on the oblateness of the Crab and the Vela pulsars are discussed.
