Hostname: page-component-cd9895bd7-lnqnp Total loading time: 0 Render date: 2024-12-27T07:32:47.391Z Has data issue: false hasContentIssue false
  • English
  • Français

Towards a Pulsar Magnetosphere Model — Physical Principles

Published online by Cambridge University Press:  25 April 2016

R. R. Burman
R. R. Burman*
Affiliation:
Department of Physics, University of Western Australia
Get access Rights & Permissions [Opens in a new window]

Extract

I shall outline the physical principles on which I believe pulsar magnetosphere models should be based. The principles follow from the equations of continuity and motion for each species and the two sourceless members of Maxwell’s set of equations, together with the steady-rotation constraint and boundary conditions at the stellar surface.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 4 , Issue 2 , 1981 , pp. 217 - 219
Copyright
Copyright © Astronomical Society of Australia 1981

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Burman, R. R.Aust. J. Phys. 33, 771 (1980).Google Scholar
Burman, R. R., ‘Inertial development of vorticity in pulsar magneto-spheres’. Aust. J. Phys. 34, in press (1981a).Google Scholar
Burman, R. R., ‘Corotation and poloidal flow in pulsar magneto-spheres’. Aust. J. Phys. 34, in press (1981b).CrossRefGoogle Scholar
Burman, R. R., and Mestel, L. Aust. J. Phys. 31, 445.Google Scholar
Burman, R. R., and Mestel, L. Aust. J. Phys. 32, 681.Google Scholar
Endean, V. G. Nature Phys. Sci. 237, 72 (1972).CrossRefGoogle Scholar
Holloway, N. J. Nature Phys. Sci. 246, 6 (1973).Google Scholar
Mestel, L. Nature Phys. Sci. 233, 149 (1971).Google Scholar