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Simultaneous solar flare observations with SDO and RHESSI provide spatiallyresolved information about hot plasma and energetic particles in flares. RHESSIallows the properties of both hot (> 8 MK) thermal plasma and nonthermalelectron distributions to be inferred, while SDO/AIA is more sensitive to lowertemperatures. We present and implement a new method to reconstruct electrondistribution functions from SDO/AIA data. The combined analysis of RHESSI andAIA data allows the electron distribution function to be inferred over thebroad energy range from ~0.1 keV up to a few tens of keV. The analysis of twowell observed flares suggests that the distributions in general agree to withina factor of three when the RHESSI values are extrapolated into the intermediaterange 1-3 keV, with AIA systematically predicting lower electron distributions.Possible instrumental and numerical effects, as well as potential physicalorigins for this discrepancy are discussed. The inferred electron distributionfunctions in general show one or two nearly Maxwellian components at energiesbelow ~ 15 keV and a non-thermal tail above.

Electron Distribution Functions in Solar Flares from combined X-ray and EUV Observations