Microwave and Hard X-ray Imaging Observations of Energetic Electrons in Solar Flares: Event of 2003 June 17

Details Microwave and Hard X-ray Imaging Observations of Energetic Electrons in Solar Flares: Event of 2003 June 17 Microwave and Hard X-ray Imaging Observations of Energetic Electrons in Solar Flares: Event of 2003 June 17

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.1306k&link_type=abstract

American Astronomical Society, SPD meeting #37, #13.06; Bulletin of the American Astronomical Society, Vol. 38, p.241

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Scientific paper

We discuss one large flare using simultaneous observations obtained with two instruments--Nobeyama Radio Heliograph (NoRH) at 17 and 34 GHz, and Reuven Ramaty High Energy Solar Spectroscopic imager (RHESSI) in the context of flare models. As we know energetic electrons accelerated to nonthermal energies are seen via microwave and hard X-ray emission from the solar corona. Imaging observations are necessary to study the energetic electrons in flare events. Nonthermal microwave emission during large solar flares is produced by gyrosynchrotron mechanism which involves coronal magnetic fields of at least a few hundred gauss and electrons of energy of a few hundred keV. Hard X-ray emission, on the other hand, is produced by bremsstrahlung from beamed or trapped electrons of a few to hundreds of keV energy. The two different methods of mapping energetic flare electrons therefore complement each other, and provide good means of testing flare models which have been abundant in the recent literature. The RHESSI HXR and NoRH microwave imaging observations of the flare of 2003 June 17 are used here as an example. The flare in question was of class M6.8, and it was observed in AR 10386, a beta-gamma-delta region, two days after its east-limb passage.

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