Hostname: page-component-848d4c4894-2xdlg Total loading time: 0 Render date: 2024-06-24T16:46:46.706Z Has data issue: false hasContentIssue false
  • English
  • Français

Propagation of Large Amplitude Pulsar Waves

Published online by Cambridge University Press:  14 August 2015

E. Asséo ,
X. Llobet  and
R. Pellat
E. Asséo
Affiliation:
Centre de Physique Théorique, Ecole Polytechnique, 91128 Palaiseau Cedex, France
X. Llobet
Affiliation:
Centre de Physique Théorique, Ecole Polytechnique, 91128 Palaiseau Cedex, France
R. Pellat
Affiliation:
Centre de Physique Théorique, Ecole Polytechnique, 91128 Palaiseau Cedex, France

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.

Large amplitude waves (hereafter l.a.w.) have been studied mainly in connection with pulsars. A rotating neutron star, with an intense non-aligned magnetic dipole field, surrounded by a vacuum, radiates beyond the light cylinder distance, large amplitude electromagnetic vacuum waves of very low frequency (Ostriker and Gunn, 1969). In such a rotating configuration electromagnetic effects completely dominate and imply the existence of a relativistic plasma in the pulsar magnetosphere (Goldreich and Julian, 1969). Because the oblique vacuum model predicts a value of 3 for the braking index of the pulsar whereas the observed or computed values are different, a realistic model has to include both the relativistic plasma outflow and the electromagnetic wave emission. The vacuum wave model has been changed to include self-consistent plasma effects (Asséo et al., 1975; Asséo et al., 1978) in plane geometry and inhomogeneities linked to spherical geometry (Asséo et al., 1981). This results in very restrictive conditions for the possibility of propagation of the l.a.w.

Type
I. Electrodynamics of the Pulsar Magnetosphere and Wave Zone
Information
Symposium - International Astronomical Union , Volume 95: Pulsars , 1981 , pp. 53 - 56
Copyright
Copyright © Reidel 1981 

References

Arons, J. and Scharlemann, E.T.: 1979, Astrophys. J. 231, p. 854.CrossRefGoogle Scholar
Asséo, E., Kennel, F.C., and Pellat, R.: 1975, Astron. Astrophys. 44, p. 31.Google Scholar
Asséo, E., Kennel, F.C., and Pellat, R.: 1978, Astron. Astrophys. 65, p. 401.Google Scholar
Asséo, E., Llobet, X., and Pellat, R.: 1981, to be submitted.Google Scholar
Cheng, A.F. and Ruderman, M.A.: 1977, Astrophys. J. 212, p. 800.CrossRefGoogle Scholar
Goldreich, P. and Julian, W.H.: 1969, Astrophys. J. 157, p. 869.CrossRefGoogle Scholar
Kennel, C.F. and Pellat, R.: 1978, J. Plasma Phys. 222, p. 297.Google Scholar
Ostriker, J.P. and Gunn, J.E.: 1969, Astrophys. J. 157, p. 1395.CrossRefGoogle Scholar
Ruderman, M.A. and Sutherland, P.G.: 1975, Astrophys. J. 196, p. 51.CrossRefGoogle Scholar
Shklovsky, I.S.: 1970, Astrophys. J. Letters 159, p. L77.CrossRefGoogle Scholar
Sturrock, P.A.: 1971, Astrophys. J. 164, p. 529.CrossRefGoogle Scholar