Nonthermal Electrons Accelerated in Solar Flare Loops

Details Nonthermal Electrons Accelerated in Solar Flare Loops Nonthermal Electrons Accelerated in Solar Flare Loops

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999spro.proc..361y&link_type=abstract

Solar Physics with Radio Observations, Proceedings of the Nobeyama Symposium, held in Kiyosato, Japan, Oct. 27-30, 1998, Edited

Physics

Scientific paper

A C9.2 flare occurred on the southeast limb (S20E90) on 1993 November 30. This flare was observed in hard X-rays and microwaves simultaneously, and its spatial structure is well resolved. Three kinds of microwave sources are located at the top and nearly at the both ends of a soft X-ray magnetic loop. The microwave source at the loop top has the following characteristics. Its time profile is basically impulsive, and its brightness temperature is 8e6K at the peak time. The degree of polarization is nearly 0%. The high brightness temperature of the microwave loop top source cannot be explained by the thermal bremsstrahlung. The most preferable mechanism for the microwave loop top emission is gyrosynchrotron emission from MeV-electrons accelerated in a weak magnetic field (a few tens Gauss). The peak time lags behind those of the other microwave sources at the footpoints of the loop. This time delay is probably caused by the trapping of the MeV-electrons in the magnetic loops. In addition, the time variation of the microwave source is similar to that of the hard X-ray one at the northern end of the magnetic loop, but the time variation of the microwave source is not similar to that of the hard X-ray ones at the southern end. This fact suggests the difference of trapping/ precipitation efficiencies of the accelerated electrons between the both ends of magnetic loops.

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