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Reviews of topical problems


Superfluidity and the magnetic field of pulsars

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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.

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Fulltext is also available at DOI: 10.1070/PU1991v034n07ABEH002446
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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Îðèãèíàë: Ñåäðàêÿí Ä Ì, Øàõàáàñÿí Ê Ì «Ñâåðõòåêó÷åñòü è ìàãíèòíîå ïîëå ïóëüñàðîâ» ÓÔÍ 161 (7) 3–40 (1991); DOI: 10.3367/UFNr.0161.199107a.0003

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