The propagation of electron fluxes in the solar corona
The problem of energetic electron flux propagation in the solar coronal plasma is solved with due regard for the influence of the oppositely directed neutralizing cold electron flux and the kinematic escape effect of the electrons with different velocities. It is shown that the flux electrons are accelerated in the process of propagation, thus forming a beam, whose velocity is constant on rather long time scales. Three regimes can be realized in this case. In the first regime, plasma waves do not have time to be excited because they escape rapidly from resonance with the beam. In the second regime, waves are excited, but the beam does not have time to relax. The third regime is quasi-linear relaxation.
The generation of solar type III radio bursts in the second regime of electron flux propagation is considered.
KeywordsPlasma Wave Solar Corona Electron Flux Radio Burst Energetic Electron
Unable to display preview. Download preview PDF.
- Ivaov, A. A., Kozorovitsky, L. L., and Rusanov, V. D.: 1969,Dokl. Akad. Nauk 184, 811.Google Scholar
- Ivanov, A. A.: 1977,The Physics of a Strongly Nonequilibrium Plasma, Nauka, Moscow (in Russian).Google Scholar
- Kaplan, S. A. and Tsytovich, V. N.: 1972,Plasma Astrophysics, Nauka, Moscow (in Russian).Google Scholar
- Kaplan, S. A., Pikelner, S. B., and Tsytovich, V. N.: 1977,Plasma Physics of the Solar Atmosphere, Nauka, Moscow (in Russian).Google Scholar
- Lin, R. P.: 1985,Solar Phys. 100, 537.Google Scholar
- Melrose, D. B.: 1974,Solar Phys. 38, 205.Google Scholar
- Melrose, D. B.: 1990,Solar Phys. 130, 3.Google Scholar
- Wild, J. P. and Smerd, F.: 1972,Ann. Rev. Astron. Astrophys. 10, 159.Google Scholar
- Zheleznyakov, V. V. and Zaitsev, V. V.: 1970,Astron. Zh. 47, 60.Google Scholar