  The evolution of inclination angle and precession damping of radio pulsars is
considered. It is assumed that the neutron star consists of 3 "freely" rotating
components: the crust and two core components, one of which contains pinned
superfluid vortices. We suppose that each component rotates as a rigid body.
Also the influence of the small-scale magnetic field on the star's braking
process is examined. Within the framework of this model the star simultaneously
can have glitch-like events combined with long-period precession (with periods
$10-10^{4}$ years). It is shown that the case of the small quantity of pinned
superfluid vortices seems to be more consistent with observations.
