Superfluidity and the magnetic field of pulsars

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.

PACS: 97.60.Gb, 97.60.Jd, 26.60.+c, 97.10.Ld, 97.10.Cv (all)
DOI: 10.1070/PU1991v034n07ABEH002446
URL: https://ufn.ru/en/articles/1991/7/a/
Citation: Sedrakyan D M, Shakhabasyan K M "Superfluidity and the magnetic field of pulsars" Sov. Phys. Usp. 34 (7) 555–571 (1991)

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RT Journal
T1 Superfluidity and the magnetic field of pulsars
A1 Sedrakyan,D.M.
A1 Shakhabasyan,K.M.
PB Physics-Uspekhi
PY 1991
FD 10 Jul, 1991
JF Physics-Uspekhi
JO Phys. Usp.
VO 34
IS 7
SP 555-571
DO 10.1070/PU1991v034n07ABEH002446
LK https://ufn.ru/en/articles/1991/7/a/

Оригинал: Седракян Д М, Шахабасян К М «Сверхтекучесть и магнитное поле пульсаров» УФН 161 (7) 3–40 (1991); DOI: 10.3367/UFNr.0161.199107a.0003