Acceleration through X-type coalescence in a small energetic flare

Details Acceleration through X-type coalescence in a small energetic flare Acceleration through X-type coalescence in a small energetic flare

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989soph..123..389s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 123, no. 2, 1989, p. 389-392.

Physics

17

Coalescing, Solar Flares, Solar Radio Bursts, Solar X-Rays, Electron Density (Concentration), Microwaves, Solar Magnetic Field, Synchrotron Radiation, X Ray Spectra

Scientific paper

The acceleration conditions in the small but fairly energetic flare of May 21, 1984 at 13:26 UT are studied. The most pronounced aspect of this flare was a series of 13 microwave/X-ray spikes, each lasting for about 0.1 sec. A previous study has shown that each of these was due to a series of successive sudden formations of small plasma knots of high-energy particles. Each of these knots lost its energy in about 50 msec. These knots can originate by the process of X-type (three-dimensional) flux-tube coalescence. The predicted rise time (30-50 msec) and energy are in good agreement with the observationally derived parameters.

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