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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/1397

Title: Toward an empirical theory of pulsar emission. VI - The geometry of the conal emission region
Authors: Rankin, J.M.
Keywords: PULSARS, RADIO ASTRONOMY
RADIO EMISSION
STELLAR MAGNETIC FIELDS
STELLAR ROTATION
Issue Date: Mar-1993
Publisher: The University of Chicago Press for the American Astronomical Society
Citation: Astrophysical Journal, 1993, Vol.405, p285-297
Abstract: An 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.
URI: http://hdl.handle.net/2289/1397
ISSN: 0004-637X
1538-4357 (online)
Alternative Location: http://adsabs.harvard.edu/cgi-bin/bib_query?1993ApJ...405..285R
Copyright: (1993) by the American Astronomical Society. Scanned images provided by the NASA ADS Data System.
Appears in Collections:Research Papers (A&A)

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