Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..149..279l&link_type=abstract
Solar Physics, vol. 149, no. 2, p. 279-288
Astronomy and Astrophysics
Astronomy
4
Electron Beams, Electron Distribution, Electron Emission, Electron Flux Density, Flux (Rate), Plasma Waves, Plasma-Particle Interactions, Solar Corona, Solar Electrons, Solar Wind, Type 3 Bursts, Wave Propagation, Distribution Functions, Electron Acceleration, Electron Energy, Plasma Heating, Radio Astronomy
Scientific paper
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 3 radio bursts in the second regime of electron flux propagation is considered.
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