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Many particles are accelerated during solar flares. To understand theacceleration and propagation processes of electrons, we require the pitch-angledistributions of the particles. The pitch angle of accelerated electrons hasbeen estimated from the propagation velocity of a nonthermal microwave sourcearchived in Nobeyama Radioheliograph data. We analyzed a flare event (anM-class flare on 2014 October 22) showing cyclical microwave brightenings atthe two footpoint regions. Assuming that the brightenings were caused by theaccelerated electrons, we approximated the velocity parallel to the magneticfield of the accelerated electrons as 77,000 and 90,000 km/s. The estimatedpitch angle of the accelerated electrons is 69-80 degrees and the size of theloss cone at the footpoint (estimated from the magnetic field strength in thenonlinear force-free field model) is approximately 43 degrees. Most of theaccelerated electrons could be reflected at the footpoint region. This featurecan be interpreted as brightenings produced by bouncing motion of theaccelerated electrons.

Characteristics of the Accelerated Electrons Moving along the Loop Derived from Cyclical Microwave Brightenings at the Footpoints