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dc.contributor.authorBhattacharya, D.-
dc.date.accessioned2005-12-29T06:01:38Z-
dc.date.available2005-12-29T06:01:38Z-
dc.date.issued1995-
dc.identifier.citationJournal of Astrophysics and Astronomy, 1995, Vol. 16, p217-232.en
dc.identifier.issn0250-6335-
dc.identifier.urihttp://hdl.handle.net/2289/961-
dc.descriptionDiamond jubilee symposium on pulsars,14-17 March 1994, RRI, Bangalore.en
dc.description.abstractObservational evidence, and theoretical models of the magnetic field evolution of neutron stars is discussed. Observational data indicates that the magnetic field of a neutron star decays significantly only if it has been a member of a close interacting binary. Theoretically, the magnetic field evolution has been related to the processing of a neutron star in a binary system through the spin evolution of the neutron star, and also through the accretion of matter on the neutron star surface. I describe two specific models, one in which magnetic flux is expelled from the superconducting core during spin-down, via a copuling between Abrikosov fluxoids and Onsager-Feynman vortices; and another in which the compression and heating of the stellar crust by the accreted mass drastically reduces the ohmic decay time scale of a magnetic field configuration confined entirely to the crust. General remarks about the behaviour of the crustal field under ohmic diffusion are also made.en
dc.format.extent1403742 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherIndian Academy of Sciences, Bangalore, India.en
dc.rightsIndian Academy of Sciences, Bangalore, India.en
dc.subjectNeutron stars;en
dc.subjectpulsars;en
dc.subjectmagnetic field;en
dc.titleThe evolution of the magnetic fields of neutron starsen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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