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Deriving a well-constrained differential emission measure (DEM) distributionfor solar flares has historically been difficult, primarily because no singleinstrument is sensitive to the full range of coronal temperatures observed inflares, from $\lesssim$2 to $\gtrsim$50 MK. We present a new technique,combining extreme ultraviolet (EUV) spectra from the EUV Variability Experiment(EVE) onboard the Solar Dynamics Observatory with X-ray spectra from the ReuvenRamaty High Energy Solar Spectroscopic Imager (RHESSI), to derive, for thefirst time, a self-consistent, well-constrained DEM for jointly-observed solarflares. EVE is sensitive to ~2-25 MK thermal plasma emission, and RHESSI to$\gtrsim$10 MK; together, the two instruments cover the full range of flarecoronal plasma temperatures. We have validated the new technique on artificialtest data, and apply it to two X-class flares from solar cycle 24 to determinethe flare DEM and its temporal evolution; the constraints on the thermalemission derived from the EVE data also constrain the low-energy cutoff of thenon-thermal electrons, a crucial parameter for flare energetics. The DEManalysis can also be used to predict the soft X-ray flux in the poorly-observed~0.4-5 nm range, with important applications for geospace science.

Constraining Solar Flare Differential Emission Measures with EVE and RHESSI