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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/2577
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dc.contributor.authorBhattacharya, D.-
dc.contributor.authorSrinivasan, G.-
dc.date.accessioned2007-06-04T08:51:04Z-
dc.date.available2007-06-04T08:51:04Z-
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, p235-242en
dc.identifier.urihttp://hdl.handle.net/2289/2577-
dc.descriptionRestricted Access.en
dc.description.abstractStatistics of observed plerions (filled supernova remnants) are used here to place some constraints on the periods of pulsars at birth. Two different scenarios for the expansion of the nebular boundary are considered, using the distribution of derived magnetic field for known pulsars in both cases. From the extremely poor association between pulsar and supernova remnants and the paucity of centrally filled synchrotron nebulae, it is concluded that the majority of neutron stars must be born spinning rather slowly, with initial rotation periods greater than about 100 milliseconds.en
dc.format.extent354618 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherReidelen
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?1987hepa.proc..235Ben
dc.rights1987 Reidelen
dc.subjectPulsarsen
dc.subjectStellar evolutionen
dc.subjectStellar rotationen
dc.subjectSupernova Remnantsen
dc.subjectCrab nebulaen
dc.subjectNeutron starsen
dc.subjectStellar envelopsen
dc.subjectStellar mass ejectionen
dc.titleOn the association between supernova remnants and pulsarsen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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