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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/1397
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dc.contributor.authorRankin, J.M.-
dc.date.accessioned2006-07-05T10:22:39Z-
dc.date.available2006-07-05T10:22:39Z-
dc.date.issued1993-03-
dc.identifier.citationAstrophysical Journal, 1993, Vol.405, p285-297en
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/1397-
dc.description.abstractAn empirical analysis of the geometry of the conal emission region for a total population of some 150 pulsars for which an adequate body of observations now exists is presented. Special attention is given to the five-component (M) class and to those other, entirely conal species which are closely related to it: the conal triple and the conal quadruple. The conal emission geometry of this group of five-component (M) stars is considered. Their two pairs of conal components suggest that both an 'inner' and 'outer' hollow conal beam is emitted. The conal emission radii of the five-component M pulsars exhibit a strikingly orderly behavior. The 'inner' and 'outer' radii have the following dependences at 1 GHz: 4.3 deg P exp -1/2 and 5.8 deg P exp -1/2, respectively, where P is the pulsar period. The other species also exhibit great regularity in their conal emission geometry.en
dc.format.extent2716703 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherThe University of Chicago Press for the American Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?1993ApJ...405..285Ren
dc.rights(1993) by the American Astronomical Society. Scanned images provided by the NASA ADS Data System.en
dc.subjectPULSARS, RADIO ASTRONOMYen
dc.subjectRADIO EMISSIONen
dc.subjectSTELLAR MAGNETIC FIELDSen
dc.subjectSTELLAR ROTATIONen
dc.titleToward an empirical theory of pulsar emission. VI - The geometry of the conal emission regionen
dc.typeArticleen
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