Dynamics of Coronal Magnetic Fields Inferred from Multi-Frequency Radio Observations of a Solar Flare

Details Dynamics of Coronal Magnetic Fields Inferred from Multi-Frequency Radio Observations of a Solar Flare Dynamics of Coronal Magnetic Fields Inferred from Multi-Frequency Radio Observations of a Solar Flare

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..229c&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Computer Science

Scientific paper

We report multi-frequency observations of a solar GOES M1.5 class flare, occurred November 5, 1998 at about 1335 UT. The microwave observations were obtained by the Solar Radio Polarimeter at 7 GHz (Itapetinga/Brazil) with high sensitivity and time resolution. The 2D decimetric-metric radio images were made with Nancay Radio Heliograph. The hard X ray data are from BATSE/CGRO and HXT from YOHKOH. Radio spectral information was obtained from RSTN data. Thus, the event was observed over a wide range of altitudes, between the low corona where 200 keV hard X rays from non-thermal electrons are produced, up to about 0.5 Ro, where the electron beams propagated outward. We discuss these observations in terms of the relation between the production of non-thermal electrons in the low /middle solar atmosphere and the dynamics of the high corona magnetic field traced by spatially resolved dm/metric emitting sources. The analysis of the 2D metric/decimetric images, associated to the fast structures in the time profiles at 7 GHz and hard X rays suggests a very complex magnetic configuration during the flare evolution. The results suggest the presence of various emitting sources at high altitudes, probably associated to different injections of non-thermal electrons. There is a suggestion that the energy release could start in the high corona by the interaction of large scale magnetic loops.

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