Particle Acceleration and Magnetic Reconnection in Solar Flares

Details Particle Acceleration and Magnetic Reconnection in Solar Flares Particle Acceleration and Magnetic Reconnection in Solar Flares

Oct 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47..691t&link_type=abstract

Publications of the Astronomical Society of Japan, v.47, p.691-697.

Astronomy and Astrophysics

Astronomy

39

Acceleration Of Particle, Magnetohydrodynamics, Sun: Flares, Sun: Magnetic Fields, Sun: X-Rays

Scientific paper

Yohkoh soft X-ray observations show that magnetic reconnection with attached slow shock heats reconnected flux tubes, and that these reconnected loops are subsequently filled with evaporated plasmas that are seen as soft X-ray loops. Hard X-ray observations show that hard X-ray (> 40--50 keV) sources are located at the footpoints of the soft X-ray loop, suggesting non-thermal electron acceleration in the loops. From these two key observations we propose a model in which a fast downflow from the reconnection site collides with the loop, and that the resulting small-scale time-varying shear flow (vortices) at the loop top drives an oppositely directed field-aligned current (channels). The field-aligned current then generates a voltage drop ( ~ 100 keV) along the magnetic fields, generating runaway electrons. If the size of the vortices is sufficiently small, the energy and number of runaway electrons, and the time scale of acceleration, are consistent with the observations. The line broadening observed with soft X-ray crystal spectrometers would be due to vortices at the loop top rather than chromospheric evaporation.

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