Hostname: page-component-77c89778f8-swr86 Total loading time: 0 Render date: 2024-07-19T22:02:22.381Z Has data issue: false hasContentIssue false
  • English
  • Français

The Location, Spectrum and Beamwidth of Pulsar Radiation from Polar Cap Models

Published online by Cambridge University Press:  14 August 2015

B. J. Rickett  and
J. M. Cordes
B. J. Rickett
Affiliation:
University of California, San Diego
J. M. Cordes
Affiliation:
Cornell University, Ithaca

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In the rotating “lighthouse” interpretation of pulsars, the average radio pulse profile is generally assumed to be a section through the average beam shape radiated by a spinning neutron star. The radio emission received in any one particular period usually differs markedly from the average profile. Such variations have been classified as subpulses (~ 3 ms) and micropulses (~ .3 ms); see Cordes (1979) for examples. However, there is not general agreement as to whether these variations are caused by the rotation of a steady narrow beam or by temporal variations of a wider beam. We first discuss these questions independently of the emitting particle location, and then apply them to a particular model.

Type
II. Radio Emission Mechanism
Information
Symposium - International Astronomical Union , Volume 95: Pulsars , 1981 , pp. 107 - 109
Copyright
Copyright © Reidel 1981 

References

Bartel, N., Sieber, W., and Graham, D.: 1980, Astron. Astrophys. 88, (in press).Google Scholar
Boriakoff, V.: 1980, 149th meeting of A.A.S., Washington, D.C. Google Scholar
Cordes, J.M.: 1979, Space Sci. Rev. 24, pp 567–600.CrossRefGoogle Scholar
Ruderman, M.A. and Sutherland, P.G.: 1975, Astrophys. J. 196, pp 51–72.CrossRefGoogle Scholar