  We investigate the neutron stars spin evolution (breaking, inclination angle
evolution and radiative precession), taking into account the superfluidity of
the neutrons in the star core. The neutron star is treated as a two-component
system consisting of a "charged" component (including the crust and the core
protons, electrons and normal neutrons) and a core superfluid neutron
component. The components are supposed to interact through the mutual friction
force. We assume that the "charged" component rotates rigidly. The neutron
superfluid velocity field is calculated directly from linearized hydrodynamical
equations. It is shown that the superfluid core accelerates the evolution of
inclinaton angle and makes all pulsars evolve to either orthogonal or coaxial
state. However, rapid evolution seems to contradict the observation data.
Obtained results together with the observations may allow to examine the
superfluid models.
