  We discuss the nature of the various modes of pulsation of superfluid neutron
stars using comparatively simple Newtonian models. The matter in these stars is
described in terms of a two-fluid model, where one fluid is the neutron
superfluid, which is believed to exist in the core and inner crust of mature
neutron stars, and the other fluid represents a conglomerate of all other
constituents (crust nuclei, protons, electrons, etc.). In our model, we
incorporate the non-dissipative interaction due to the so-called entrainment
effect, whereby the momentum of one constituent (e.g. the neutrons) carries
along part of the mass of the other constituent. We show that there is no
independent set of propagating g-modes in a superfluid neutron star core. We
also approach the toroidal pulsation modes of a slowly rotating superfluid
star. We show that the superfluid equations support a new class of r-modes.
Finally, the role of the entrainment effect on the superfluid mode frequencies
is shown explicitly via solutions to local dispersion relations.
