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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/2592
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dc.contributor.authorRadhakrishnan, V.-
dc.contributor.authorShukre, C.S.-
dc.date.accessioned2007-06-04T11:27:40Z-
dc.date.available2007-06-04T11:27:40Z-
dc.date.issued1987-
dc.identifier.citationHigh energy phenomena around collapsed stars; Proceedings of the NATO Advanced Study Institute, Cargese, France, Sept. 2-13, 1985, Dordrecht, D. Reidel Publishing Co., 1987, p271-278en
dc.identifier.urihttp://hdl.handle.net/2289/2592-
dc.descriptionRestricted Access.en
dc.description.abstractAnalysis of a sample of pulsar proper-motions leads to the conclusion that most pulsars were born in and released from binary systems. A minority of pulsars belong to a class characterized by low velocities and low magnetic fields. These were significantly spun-up by accretion and released from the binary through a nonexplosive disruption of the companion. The rest belong to the high-velocity, high-magnetic field class. Using relations between the speeds at present and those in the binary orbit prior to its disruption, it is shown that such binaries must have undergone a common envelope phase of stellar evolution. The limits obtained on the masses and separations of these binary systems conform closely with those from stellar-evolution theory.en
dc.format.extent327150 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherReidelen
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?1987hepa.proc..271Ren
dc.rights1987 Reidelen
dc.subjectBinary starsen
dc.subjectPulsarsen
dc.subjectStellar evolutionen
dc.subjectStellar modelsen
dc.subjectStellar motionsen
dc.subjectStellar envelopsen
dc.subjectStellar magnetic fieldsen
dc.subjectStellar mass accretionen
dc.titleThe binary origin of pulsar velocitiesen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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