Statistical Properties of Super-Hot Solar Flares Amir Caspi †1*, Säm Krucker 2,3, Robert P. Lin...
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3 Flare Selection Analysis was restricted to only M- and X-class flares – those most likely to produce super-hot plasma. We required: Good RHESSI coverage of X-ray peak (defined as uninterrupted observation over the full 10 minutes prior to GOES SXR peak) Clearly identifiable HXR (25-50 keV) and SXR (6-12 keV) peaks, occurring in order before the GOES SXR peak Time-series spectra fit reasonably well by the model (below) Imageable with grid 3 (~7 arcsec FWHM) using CLEAN 260 analyzable flares during (234 M, 26 X) 37 flares chosen in simple chronological order (25 M [from 2002], 12 X [from ]) – see Table 1
