  Modeling the dynamics of the quantum fluids within a spinning-down neutron
star gives a description consistent with observed pulsar magnetic field
evolution and spin-period "glitches." The long-standing problem of large
predicted excesses in spin-down sustained pulsar heating from such models now
see ms resolvable. However, the origin of some pulsar spin-period and
pulse-shape modulations which have been interpreted as manifestations of very
long period (~year) stellar precession is a crucial challenge to canonical
neutron star models.
