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Quasi-Linear Dynamics of a Hot Maxwellian Electron Distribution Released from a Localized Region in a Homogeneous Plasma

Published online by Cambridge University Press:  14 August 2015

R.J.-M. Grognard
R.J.-M. Grognard*
Affiliation:
Division of Radiophysics, CSIRO, Sydney, Australia

Abstract

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To investigate by numerical analysis the transition towards the asymptotic regime postulated by Ryutov and Sagdeev (1970) in their study of the expansion of a hot electron cloud through a plasma, a physically consistent system of one-dimensional quasi-linear equations has been solved on a Cyber 7600. The results obtained for various conditions of injection were all found in qualitative agreement with the simple analytic description of Ryutov and Sagdeev, in spite of the serious deficiencies of their analysis. Although the aims and techniques of the present study are quite distinct from published numerical works by Takakura and Shibahashi (1976) and Magelssen (1976), all the results point towards the same conclusion: plasmon emission, due to advective instability at the front of the electronic disturbance, is followed by strong reabsorption through a reverse advective process at the rear. In the present note, only the case of a localized hot electronic distribution (initially Maxwellian with Te = 108 K) is considered. The effect of plasmon-plasmon scattering, which can also be included in the programmes, is mentioned in the conclusion.

Type
Session V - Solar Bursts - Meter-Decameter Wavelengths
Information
Symposium - International Astronomical Union , Volume 86: Radio Physics of the Sun , 1980 , pp. 303 - 307
Copyright
Copyright © Reidel 1980 

References

Grognard, R.J.-M.: 1975, Aust. J. Phys. 28, pp. 731–753.CrossRefGoogle Scholar
Harris, E.G.: 1969, Adv. Plasma Phys. 3, pp. 157–241.Google Scholar
Magelssen, G.R.: 1976, Non Relativistic Electron Stream Propagation in the Solar Atmosphere and Solar Wind: Type III Bursts. University of Colorado and N.C.A.R. Cooperative , Boulder.Google Scholar
Magelssen, G.R., and Smith, D.F.: 1977, Solar Phys. 55, pp. 212–239.CrossRefGoogle Scholar
Ryutov, D.D., and Sagdeev, R.Z.: 1970, Sov. Phys. JETP 31, pp. 396–399.Google Scholar
Takakura, T., and Shibahashi, H.: 1976, Solar Phys. 46, pp. 323–346.CrossRefGoogle Scholar
Wild, J.P.: 1980, Proc. IAU Symp. 86 (this volume), pp. 5.CrossRefGoogle Scholar
Zaitsev, V.V., Kunilov, M.V., Mityakov, N.A., and Rapoport, V.O.: 1974, Sov. Astron. AJ 18, pp. 147–151.Google Scholar
Zaitsev, V.V., Mityakov, N.A., and Rapoport, V.O.: 1972, Solar Phys. 24, pp. 444–456.CrossRefGoogle Scholar
Zheleznyakov, V.V., and Zaitsev, V.V.: 1970, Sov. Astron. AJ 14, pp. 47–58.Google Scholar