Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-11-26T22:21:41.725Z Has data issue: false hasContentIssue false
  • English
  • Français

Hot Relativistic Winds and the Crab Nebula

Published online by Cambridge University Press:  14 August 2015

F. S. Fujimura  and
C. F. Kennel
F. S. Fujimura
Affiliation:
Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90024, USA
C. F. Kennel
Affiliation:
Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90024, USA

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.

We review efforts to construct a self-consistent model of pulsar magnetospheres that links the particle source near the pulsar to the outflowing relativistic wind and couples the wind to the surrounding nebula. Pair production source models (Sturrock, 1971; Ruderman and Sutherland, 1975; Arons, 1979) produce outflowing positronic plasmas which are too dense to support a plasma wave of relativistic amplitude (Kennel et al., 1973). Therefore an appropriate description seems to be a relativistic magnetohydrodynamic (MHD) wind. Radiation from a relativistic wind will be collimated forward and can only be observed along the line of sight to the wind source. This makes relativistic winds essentially unobservable and provides an almost invisible method of energy transport. Photons can be emitted in all directions and the existence of the wind inferred only after the wind has been decelerated by a confining shock (causing the flow to become subsonic and non-relativistic).

Type
I. Electrodynamics of the Pulsar Magnetosphere and Wave Zone
Information
Symposium - International Astronomical Union , Volume 95: Pulsars , 1981 , pp. 51 - 52
Copyright
Copyright © Reidel 1981 

References

Arons, J.: 1979, Space Sci. Rev. 24, p. 437.Google Scholar
Cheng, A. and Ruderman, M.: 1977, Astrophys. J. 216, p. 865.Google Scholar
Fujimura, F.S. and Kennel, C.: 1981, to be submitted.Google Scholar
Kennel, C.F., Schmidt, G., and Wilcox, T.: 1973, Phys. Rev. Letters 31, p. 1864.Google Scholar
Kennel, C.F., Fujimura, F.S., and Pellat, R.: 1979, Space Sci. Rev. 24, p. 407.Google Scholar
Kennel, C.F. and Fujimura, F.S.: 1981, Proc. Dumand Conference.Google Scholar
Michel, F.: 1969, Astrophys. J. 157, p. 1183.Google Scholar
Okamoto, I.: 1978, Mon. Not. R. Astr. Soc. 185, p. 69.Google Scholar
Schmidt, G.D., Angel, J.R.P., and Beaver, E.A.: 1979, Astrophys. J. 227, p. 106.Google Scholar
Ruderman, M. and Sutherland, P.: 1975, Astrophys. J. 196, p. 51.Google Scholar
Sturrock, P.: 1971, Astrophys. J. 164, p. 529.Google Scholar