Other
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640401c&link_type=abstract
American Astronomical Society, AAS Meeting #216, #404.01; Bulletin of the American Astronomical Society, Vol. 41, p.899
Other
Scientific paper
It is well known that the radio type III bursts are closely associated with the hard X-ray (HXR) bursts in some solar flares. Generally, most HXR emission comes from nonthermal electron bremsstrahlung confined in closed field lines, while type III bursts are generated by electrons propagating outward in the corona along open field lines. Recently RHESSI has discovered HXR emission from double coronal sources in several solar flares, the upper of which is interpreted to be due to electrons accelerated above the reconnection X-point in open field lines. Here we present two such events on 2003 November 3 (X3.9 class) and 2002 October 31 (X1.2) that are accompanied with radio type III bursts. In the 2003 November 3 flare, the upper coronal source extends up to 60-80 keV and its spectrum can be fitted by a power law. The Nancay Radioheliograph sources at metric and decimetric wavelengths appear to be located above and as continuation of the upper coronal HXR source. The 2002 October 31 flare has interplanetary type III bursts observed in WIND/WAVES spectrograms but there is no imaging observation. In contrast, we present another flare on 2005 September 8 (M2.1) that has two flaring loops resolved in HXR and appears to consist of closed magnetic loops. However, the upper coronal source in this flare is associated with a closed loop and there is no drifting feature found in radio spectrograms from space or ground-based observations. Future HXR and radio telescopes of higher dynamic range may detect emission produced by the nonthermal electrons from their acceleration to propagation stages in open field line regions in more flare events.
Chen Qingrong
Petrosian Vahe
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