Spike emission at 21 CM wavelength in post-flare loops

Details Spike emission at 21 CM wavelength in post-flare loops Spike emission at 21 CM wavelength in post-flare loops

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..143..317f&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 143, no. 2, p. 317-326.

Physics

4

Coronal Loops, Solar Flares, Solar Physics, Solar Radio Emission, Electron Acceleration, Solar Electrons, Solar Magnetic Field

Scientific paper

Electron-cyclotron maser instability produced by accelerated energetic electrons is today's most favored process for spike emission on ultrashort time scales at dm wavelengths. The process of electron acceleration occurs primarily in preimpulsive and impulsive phases. We present observations of spike bursts at 21 cm in a limb event that occurred in AR 5629 on 1989 August 17. Optical observations of the event from Beijing Astronomical Observatory show coronal loops that interact just before the spike groups appeared. This implies that additional particle acceleration might be produced by the interaction between emerging loops and original large loops, and become the source of the energetic electrons responsible for the spike emission appearing in the descending phase. Some important parameters are deduced.

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