  As mature neutron stars are cold (on the relevant temperature scale), one has
to carefully consider the state of matter in their interior. The outer
kilometer or so is expected to freeze to form an elastic crust of increasingly
neutron-rich nuclei, coexisting with a superfluid neutron component, while the
star's fluid core contains a mixed superfluid/superconductor. The dynamics of
the star depend heavily on the parameters associated with the different phases.
The presence of superfluidity brings new degrees of freedom -- in essence we
are dealing with a complex multi-fluid system -- and additional features: Bulk
rotation is supported by a dense array of quantised vortices, which introduce
dissipation via mutual friction, and the motion of the superfluid is affected
by the so-called entrainment effect. This brief survey provides an introduction
to -- along with a commentary on our current understanding of -- these
dynamical aspects, paying particular attention to the role of entrainment, and
outlines the impact of superfluidity on neutron-star seismology.
