Hostname: page-component-848d4c4894-2pzkn Total loading time: 0 Render date: 2024-05-03T10:15:26.069Z Has data issue: false hasContentIssue false
  • English
  • Français

Structure of the Pulsar Magnetosphere

Published online by Cambridge University Press:  14 August 2015

L. Mestel
L. Mestel*
Affiliation:
Astronomy Centre, University of Sussex

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.

Motivation for the study of the pulsar magnetosphere is multifold. First of all, energy-wise the magnetosphere is the dominant problem, for the energy emitted in the radio pulses is at most one per-cent of the energy loss inferred from the secular increase in the rotation period of the central neutron star. With the possible exception of gamma-ray emission in a few cases, the pulsing observed in all wavelengths can be regarded as a diagnostic of a more basic phenomenon. A successful model should in fact tell us the total rate of energy loss from the star and its distribution between a low-frequency wave, a possible wind, and emission in the radio, optical, X-ray and gamma-ray bands. As a necessary preliminary, the model should predict the strength of the currents leaving and returning to the star, the location of relativistic particles, and the conditions for transition to a quantum magnetosphere via pair production (Sturrock 1971). But even if magnetospheric theory did not offer such hopes of ultimate links with observation, the problem is so well-defined that it is a challenge to the theorist: it is just intolerable that we should not know how a rotating magnetized neutron star comes to terms with its environment.

Type
I. Electrodynamics of the Pulsar Magnetosphere and Wave Zone
Information
Symposium - International Astronomical Union , Volume 95: Pulsars , 1981 , pp. 9 - 23
Copyright
Copyright © Reidel 1981 

References

Arons, J.: 1979, Space Sci. Rev. 24, p. 437.CrossRefGoogle Scholar
Burman, R.R.: 1980, Australian J. Phys. (in press).Google Scholar
Burman, R.R. and Mestel, L.: 1978, Australian J. Phys. 31, p. 455.CrossRefGoogle Scholar
Burman, R.R. and Mestel, L.: 1979, Australian J. Phys. 32, p. 681.CrossRefGoogle Scholar
Cheng, A.F. and Ruderman, M.A.: 1980, Astrophys. J. 235, p. 576.CrossRefGoogle Scholar
Cohen, J.M. and Toton, E.T.: 1971, Astrophys. Letters 7, p. 213.Google Scholar
Deutsch, A.J.: 1955, Ann. d'Astrophys. 18, p. 1.Google Scholar
Endean, V.G.: 1972, Nature Phys. Sci. 237, p. 72.CrossRefGoogle Scholar
Endean, V.G.: 1974, Astrophys. J. 187, p. 359.CrossRefGoogle Scholar
Erber, T.: 1966, Rev. Mod. Phys. 38, p. 626.CrossRefGoogle Scholar
Fawley, W.M., Arons, J., and Scharlemann, E.T.: 1977, Astrophys. J. 271, p. 227.CrossRefGoogle Scholar
Gold, T.: 1968, Nature 218, p. 73.CrossRefGoogle Scholar
Goldreich, P. and Julian, W.H.: 1969, Astrophys. J. 157, p. 869.CrossRefGoogle Scholar
Goldreich, P.: 1970, Astrophys. J. Letters 160, p. L11.CrossRefGoogle Scholar
Holloway, N.J.: 1973, Nature Phys. Sci. 246, p. 6.CrossRefGoogle Scholar
Holloway, N.J.: 1977, Mon. Not. R. Astr. Soc. 181, p. 9P.CrossRefGoogle Scholar
Jackson, E.A.: 1976a, Nature 259, p. 25 CrossRefGoogle Scholar
Jackson, E.A.: 1976b, Astrophys. J. 206, p. 831.CrossRefGoogle Scholar
Kahn, F.D.: 1971, Paper read at Royal Astronomical Society.Google Scholar
Kennel, C.F., Fujimura, F.S., and Pellat, R.: 1979, Space Sci. Rev. 24, p. 407.Google Scholar
Mestel, L.: 1971, Nature Phys. Sci. 233, p. 149.CrossRefGoogle Scholar
Mestel, L.: 1973, Astrophys. Space Sci. 24, p. 289.CrossRefGoogle Scholar
Mestel, L., Phillips, P., and Wang, Y.-M.: 1979, Mon. Not. R. Astr. Soc. 188, p. 385.CrossRefGoogle Scholar
Mestel, L. and Selley, C.S.: 1970, Mon. Not. R. Astr. Soc. 149, p. 197.CrossRefGoogle Scholar
Mestel, L. and Wang, Y.-M.: 1979, Mon. Not. R. Astr. Soc. 188, p. 799.CrossRefGoogle Scholar
Mestel, L. and Wang, Y.-M.: 1981, Mon. Not. R. Astr. Soc. (in press).Google Scholar
Mestel, L., Wright, G.A.E., and Westfold, K.C.: 1976, Mon. Not. R. Astr. Soc. 175, p. 257.CrossRefGoogle Scholar
Michel, F.C.: 1973, Astrophys. J. 180, p. 207.CrossRefGoogle Scholar
Michel, F.C.: 1974, Astrophys. J. 192, p. 713.CrossRefGoogle Scholar
Michel, F.C.: 1975, Astrophys. J. 196, p. 579.CrossRefGoogle Scholar
Michel, F.C.: 1979, Astrophys. J. 227, p. 579.CrossRefGoogle Scholar
Michel, F.C. and Goldwire, H.C.: 1970, Astrophys. Letters 5, p. 21.Google Scholar
Okamoto, I.: 1974, Mon. Not. R. Astr. Soc. 167, p. 457.CrossRefGoogle Scholar
Pacini, F.: 1967, Nature 216, p. 567.CrossRefGoogle Scholar
Pilipp, W.G.: 1974, Astrophys. J. 190, p. 391.CrossRefGoogle Scholar
Rylov, Yu.A.: 1977, Astrophys. Space Sci. 51, p. 59.CrossRefGoogle Scholar
Rylov, Yu.A.: 1979, Astrophys. Space Sci. 66, p. 401.CrossRefGoogle Scholar
Scharlemann, E.T., Arons, J., and Fawley, W.M.: 1978, Astrophys. J. 222, p. 297.CrossRefGoogle Scholar
Schmalz, R., Ruder, H., and Herold, H.: 1979, Mon. Not. R. Astr. Soc. 189, p. 709.CrossRefGoogle Scholar
Schmalz, R., Ruder, H., Herold, H., and Rossmanith, C.: 1980, Mon. Not. R. Astr. Soc. 192, p. 409.CrossRefGoogle Scholar
Sturrock, P.A.: 1971, Astrophys. J. 164, p. 529.CrossRefGoogle Scholar
Sturrock, P.A.: 1979, Paper read at IAU, Montreal.Google Scholar