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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2926
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dc.contributor.authorKapoor, R. C-
dc.contributor.authorShukre, C. S-
dc.date.accessioned2008-07-29T04:49:14Z-
dc.date.available2008-07-29T04:49:14Z-
dc.date.issued2001-08-
dc.identifier.citationAstronomy and Astrophysics, Vol. 375, No. 2, pp. 405 – 410en
dc.identifier.issn1432-0746-
dc.identifier.urihttp://hdl.handle.net/2248/2926-
dc.description.abstractA remarkably precise observational relation for pulse core component widths of radio pulsars is used to derive stringent limits on pulsar radii, strongly indicating that pulsars are strange stars rather than neutron stars. This is achieved by inclusion of general relativistic effects due to the pulsar mass on the size of the emission region needed to explain the observed pulse widths, which constrain the pulsar masses to be <=2.5 Msun and radii <=10.5 km.en
dc.format.extent151118 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherEDP Sciencesen
dc.relation.urihttp://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/abs/2001/32/aa1367/aa1367.htmlen
dc.subjectPulsars: Generalen
dc.subjectDense Matteren
dc.subjectEquation Of State: Stars : Neutronen
dc.titleAre radio pulsars strange stars?en
dc.typeArticleen
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