  We propose a possible way to solve the problem of inconsistency between the
neutron star long-period precession and superfluid vortex pinning, which is the
basis of the most successful theories of pulsar glitches. We assume that the
pinning takes place in the region of the neutron star core, which, being
magnetically decoupled, can rotate relative to the crust. In the framework of a
simple three-component model we show that these two phenomena can coexist in
the same pulsar. Some constraints on the formally introduced interaction
coefficients following from observation data are formulated.
