Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1974
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974soph...38..205m&link_type=abstract
Solar Physics, vol. 38, Sept. 1974, p. 205-215.
Astronomy and Astrophysics
Astronomy
15
Electron Trajectories, Electrostatic Waves, Solar Magnetic Field, Type 3 Bursts, Lines Of Force, Magnetohydrodynamic Waves, Radio Sources (Astronomy), Wave Generation
Scientific paper
The suggestion is explored that the two-stream instability has little effect on the propagation of the electron streams which generate type III bursts because the time required (ti) for development of the instability is comparable with or greater than the time available (Delta t) for growth of the waves. Inferred parameters for streams in the corona and measured parameters for streams at the orbit of the earth are compatible with this suggestion. Quasi-linear relaxation, which should occur as the stream forms, ensures that the two times are equal initially, and restricts the number of escaping electrons to approximately 10 to the 31st power electrons. The minimum density requirement on the stream for the two-stream instability to occur is found to be much less restrictive than the requirement that there should be many streaming electrons per Debye sphere.
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