The current state of the theory of superfluidity in pulsars is presented. The superfluidity of hadronic matter in neutron stars is considered. It is shown that strong interaction between the neutron and proton condensates leads to a drag current of superconducting protons and to the generation of a strong time-independent magnetic field (B = 10$^{12}$ G) parallel to the axis of rotation. The strength of this field depends on the microscopic parameters of the superfluid hadrons. Models explaining the origin of glitches and postglitch relaxation are discussed. The coupling time between the neutron superfluid and the rigid crust of the neutron star is calculated.

PT Journal Article
TI Superfluidity and the magnetic field of pulsars
AU Sedrakyan D M
FAU Sedrakyan DM
AU Shakhabasyan K M
FAU Shakhabasyan KM
DP 10 Jul, 1991
TA Phys. Usp.
VI 34
IP 7
PG 555-571
RX 10.1070/PU1991v034n07ABEH002446
URL https://ufn.ru/en/articles/1991/7/a/
SO Phys. Usp. 1991 Jul 10;34(7):555-571