  In the core of a canonical spinning magnetized neutron star(NS) a nearly
uniform superfluid neutron vortex-array interacts strongly with a twisted array
of magnetic flux-tubes threading the core's superconducting protons. One
consequence is that changes in NS-spin alter both arrays and also the magnetic
field distribution on the surface of the surrounding crust. Among predicted
consequences for very young spinning-down NSs are "spin-down indices"
increasing from 2 to 3, and a family of (Crab-like) spin-period "glitches" with
permanent fractional jumps in spin-down torque 10E5 times greater than those in
NS-spin. For older NSs, average spin-down indices increase to around 5, and an
additional (Vela-like) family of giant glitches develops. NS spin-up to
millesecond pulsars results in a high abundance of orthogonal and aligned
rotators, and anomolously small polar cap areas. Observations do not conflict
with these expectations. An epoch of NS magnetic field evolution between the
onset of proton superconductivity (approx. yr) and neutron superfluidity
(approx. 10E3 yrs ?) may be important for large surface magnetic field changes
and needs further study. Observations generally considered evidence for NS
precession seem to need reconsideration.
