STEREO and RHESSI Observations of Electron Acceleration in a Partially Disk-Occulted Solar Flare

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Scientific paper

RHESSI hard X-ray observations of partially-disk occulted solar flares provide crucial information on faint coronal hard X-ray sources in the absence of generally much brighter emissions from footpoints of flare loops. Coronal hard X-ray sources can differ fundamentally from the classical footpoint sources of the flare impulsive phase and provide unique information about the supra-thermal electrons closest to the site in the corona where their acceleration is believed to occur. The different view-angles provided by the STEREO spacecraft allow us to put the partially occulted hard X-ray sources observed by RHESSI in context with the EUV flare ribbons and the EUV emission from CME observed by STEREO/EUVI.
In this presentation we report on the GOES C8 flare observed on December 31, 2007 peaking around 01:11UT. From Earth-view (RHESSI), the flare occurs about 12 degrees behind the eastern limb giving an occultation height of 16 Mm. From STEREO B, the flare ribbons are seen on the disk (about 10 degrees from the limb), while the flare is highly occulted (130 Mm) for STEREO A observations so that emissions related to the associated CME are seen. Despite the occultation, RHESSI observes strong non-thermal emissions up to 100 keV that entirely originate from the corona. Initially, the coronal hard X-ray emission is seen from above the EUV flare ribbons similar to what is reported in the Masuda flare. Later on, emissions from a radially extended (approximately 20 Mm) source is seen. The radial extension is in the same direction as the current sheet of the outward moving CME suggesting that the HXR emission might be a direct signature of electrons accelerated in the reconnection process.

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