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Article: Magnetic field decay from the core of neutron stars: Effects of interpinning of 3P2 neutron superfluid and 1S0 proton superconducting fluid

TitleMagnetic field decay from the core of neutron stars: Effects of interpinning of 3P2 neutron superfluid and 1S0 proton superconducting fluid
Authors
KeywordsConduction
Dense Matter
Mhd
Pulsars: General
Stars: Neutron
Issue Date1993
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1993, v. 408 n. 1, p. 167-178 How to Cite?
AbstractWe consider a mechanism by which most of the magnetic field in the core of a spinning-down neutron star can be driven out from the core on a time scale of a few million years but will leave a residual field ≥ 108 G on the Hubble time scale (∼3 × 1010 yr). Such a driving force arises from the fact that the magnetized vortices of the 3P2 neutron superfluid are effectively pinned by the magnetic fluxoids of the 1S0 proton superconducting fluid. Despite the strong magnetic pinning energy, ∼10 MeV per intersection, the neutron vortices and the proton fluxoids do not always move out with the same speed because the combined effects of the magnus force, buoyancy force, tension of the fluxoids, drag force, and thermal activation allow the neutron vortices and proton fluxoids to creep through each other in a manner analogous to the creeping phenomenon in a type II superconductor. In this paper, we ignore the collective effects of the drag force and show how the core field decay depends on the decay of the crustal current. In addition to the decay of the pulsar magnetic field such core fluxoid motion may also play a crucial role in other pulsar phenoma.
Persistent Identifierhttp://hdl.handle.net/10722/174912
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorDing, KYen_US
dc.contributor.authorCheng, KSen_US
dc.contributor.authorChau, HFen_US
dc.date.accessioned2012-11-26T08:48:05Z-
dc.date.available2012-11-26T08:48:05Z-
dc.date.issued1993en_US
dc.identifier.citationAstrophysical Journal Letters, 1993, v. 408 n. 1, p. 167-178en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174912-
dc.description.abstractWe consider a mechanism by which most of the magnetic field in the core of a spinning-down neutron star can be driven out from the core on a time scale of a few million years but will leave a residual field ≥ 108 G on the Hubble time scale (∼3 × 1010 yr). Such a driving force arises from the fact that the magnetized vortices of the 3P2 neutron superfluid are effectively pinned by the magnetic fluxoids of the 1S0 proton superconducting fluid. Despite the strong magnetic pinning energy, ∼10 MeV per intersection, the neutron vortices and the proton fluxoids do not always move out with the same speed because the combined effects of the magnus force, buoyancy force, tension of the fluxoids, drag force, and thermal activation allow the neutron vortices and proton fluxoids to creep through each other in a manner analogous to the creeping phenomenon in a type II superconductor. In this paper, we ignore the collective effects of the drag force and show how the core field decay depends on the decay of the crustal current. In addition to the decay of the pulsar magnetic field such core fluxoid motion may also play a crucial role in other pulsar phenoma.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectConductionen_US
dc.subjectDense Matteren_US
dc.subjectMhden_US
dc.subjectPulsars: Generalen_US
dc.subjectStars: Neutronen_US
dc.titleMagnetic field decay from the core of neutron stars: Effects of interpinning of 3P2 neutron superfluid and 1S0 proton superconducting fluiden_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.emailChau, HF: hfchau@hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.identifier.authorityChau, HF=rp00669en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-12044253848en_US
dc.identifier.volume408en_US
dc.identifier.issue1en_US
dc.identifier.spage167en_US
dc.identifier.epage178en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridDing, KY=43960894500en_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridChau, HF=7005742276en_US

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