On the slow-down of the millisecond pulsar PSR 1937 + 214

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3977

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DC Field	Value	Language
dc.contributor.author	Sivaram, C	-
dc.contributor.author	Kochhar, R. K	-
dc.date.accessioned	2008-10-25T13:05:24Z	-
dc.date.available	2008-10-25T13:05:24Z	-
dc.date.issued	1984-01	-
dc.identifier.citation	Astrophysics and Space Science, Vol. 98, No. 1, pp. 203 - 205	en
dc.identifier.issn	0004-640X	-
dc.identifier.uri	http://hdl.handle.net/2248/3977	-
dc.description.abstract	There are indications that less than 10/sup-3 of the spin-down energy of the millisecond pulsar PSR 1937+214 emerges as electromagnetic radiation. The implications of this result are discussed. The surface magnetic field would then be ≡10/sup7G, making the pulsar optically undetectable, and casting aspersions on the accretion disc spin-up neutron star models for the pulsar. The pulsar should have an equatorial ellipticity ɛ ≡ 10/sup-9, which can be accounted for if the equatorial magnetic field departs from axisymmetry by one part in 10/sup3.	en
dc.language.iso	en	en
dc.publisher	Springer	en
dc.relation.uri	http://www.springerlink.com/content/q65410213g355462/	en
dc.subject	Astrophysics	en
dc.subject	Pulsars	en
dc.subject	Stellar Magnetic Fields	en
dc.subject	Accretion Disks	en
dc.subject	Electromagnetic Radiation	en
dc.subject	Energy Dissipation	en
dc.subject	Stellar Models	en
dc.subject	Stellar Rotation	en
dc.title	On the slow-down of the millisecond pulsar PSR 1937 + 214	en
dc.type	Article	en
Appears in Collections:	IIAP Publications

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