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Toward an empirical theory of pulsar emission. VI - The geometry of the conal emission region
Rankin, Joanna M.
AA(Raman Research Inst., Bangalore, India)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 405, no. 1, p. 285-297. (ApJ Homepage)
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NASA/STI Keywords:
Pulsars, Radio Astronomy, Radio Emission, Stellar Magnetic Fields, Stellar Rotation
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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.

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