Models for the evolution of neutron star magnetic fields

Bhattacharya, D.

Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/2474

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DC Field	Value	Language
dc.contributor.author	Bhattacharya, D.	-
dc.date.accessioned	2007-05-25T09:46:53Z	-
dc.date.available	2007-05-25T09:46:53Z	-
dc.date.issued	1999	-
dc.identifier.citation	Proceedings of the Netherlands Academy Colloquim, 1999, p235	en
dc.identifier.isbn	90-6984-247-5	-
dc.identifier.uri	http://hdl.handle.net/2289/2474	-
dc.description	Restricted Access. Pulsar Timing, General Relativity and the Internal Structure of Neutron Stars, Eds. Z. Arzoumanian, F. Van der Hooft, and E. P. J. van den Heuvel. Published by Koninklijke Nederlandse Akademie van Wetenschappen, Amsterdam, The Netherlands, 1999.	en
dc.description.abstract	Recent observations indicate that the magnetic field of a neutron star decays significantly only when the neutron star is in an interacting binary. This paper reviews the theoretical attempts to model such evolution. Three main possibilities are discussed: the expulsion of the magnetic flux from superconducting core during propeller spin-down in companion's wind, screening of the magnetic field by accreted matter and rapid ohmic decay of crustal magnetic field as a result of heating during accretion. It is found that the screening is unlikely to be effective because of strong Rayleigh-Taylor instabilities. The spindown-induced flux expulsion as well as the crustal heating models remain promising.	en
dc.format.extent	922318 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	en
dc.publisher	Koninklijke Nederlandse Akademie van Wetenschappen, Amsterdam	en
dc.relation.uri	http://adsabs.harvard.edu/cgi-bin/bib_query?1999ptgr.conf..235B	en
dc.rights	1999 Koninklijke Nederlandse Akademie van Wetenschappen	en
dc.title	Models for the evolution of neutron star magnetic fields	en
dc.type	Article	en
Appears in Collections:	Research Papers (A&A)

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