Radio signature of fragmented electron injection into a coronal loop

Details Radio signature of fragmented electron injection into a coronal loop Radio signature of fragmented electron injection into a coronal loop

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..153..403f&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 153, no. 1-2, p. 403-417

Astronomy and Astrophysics

Astronomy

26

Coronal Loops, Cyclotron Radiation, Electron Beams, Injection, Pulsed Radiation, Radio Astronomy, Radio Spectra, Solar Electrons, Solar Radio Emission, Wave-Particle Interactions, X Ray Spectra, Gamma Ray Observatory, Particle Acceleration, Solar Flares, X Ray Astronomy

Scientific paper

High-time resolution observations of an unusual event of 1991 November 17, 07:04 UT at 2.5 and 2.85 GHz are presented. The event demonstrates sophisticated fine time structure including sudden reductions and quasi-periodic pulsations about various `zero' levels. It is shown that the sudden reductions (approx. = 30 - 100 ms) can be produced with upward-injected greater than 100 keV electron beams filling the loss-cone. In such a case the acceleration is proceeding in a dense plasma layer with number density n greater than (2.5 x 1010)/cu cm. The shortest time scale of the fragmented injection is tauinj,min approx. = 30 ms. Several different pulsating regimes arising due to the wave-particle and wave-wave interactions are considered. A theoretical mechanism with the nonlinear oscillations of Langmuir waves at the different steady-state levels provides the best agreement with the observed pulsations. The reduced steady-state level of the second train of pulsations is connected with the long (quasi-continuous) injection of electrons filling the loss-cone, which reduced the wave energy level. Physical parameters of the radio source were obtained. On the other hand, electron-cyclotron maser (ECM) nonlinear pulsations seem to be responsible for the radio pulsations observed in dMe stars.

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