Electron cyclotron maser emission from solar flares

Details Electron cyclotron maser emission from solar flares Electron cyclotron maser emission from solar flares

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..111..155v&link_type=abstract

(Observatoire de Paris, CNRS, CNES, et al., CESRA Workshop on Particle Acceleration and Trapping in Solar Flares, 2nd, Aubigny-s

Physics

15

Electron Cyclotron Heating, High Energy Electrons, Masers, Solar Flares, Chromosphere, Electron Acceleration

Scientific paper

The characteristics of the linear and nonlinear evolution of the loss-cone and ring velocity distributions that can excite the electron cyclotron maser (ECM) are reviewed. It is shown that, depending on the ratio of plasma to gyrofrequency, different harmonics will dominate the emission. It is indicated from the nonlinear evolution of the loss cone or ring distributions that the instability will saturate in 10 to the -6th s in the solar atmosphere, and that only 1-5 percent of the available energy will be transferred to the electromagnetic waves. The present ECM model is used to explain most of the known characteristics of the millisecond spikes in solar flares. The escape of ECM radiation from the solar surface, and the interaction of the strong electromagnetic radiation with the plasma outside the radiation, are also considered.

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