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The chromospheric response to the input of flare energy is marked by extendedextreme ultraviolet (EUV) ribbons and hard X-ray (HXR) footpoints. These areusually explained as the result of heating and bremsstrahlung emission fromaccelerated electrons colliding in the dense chromospheric plasma. We presentevidence of impulsive heating of flare ribbons above 10 MK in a two-ribbonflare. We analyse the impulsive phase of SOL2013-11-09T06:38, a C2.6 classevent using data from Atmospheric Imaging Assembly (AIA) on board of SolarDynamics Observatory (SDO) and the Reuven Ramaty High Energy SolarSpectroscopic Imager (RHESSI) to derive the temperature, emission measure anddifferential emission measure of the flaring regions and investigate theevolution of the plasma in the flaring ribbons. The ribbons were visible at allSDO/AIA EUV/UV wavelengths, in particular, at 94 and 131 \AA\ filters,sensitive to temperatures of 8 MK and 12 MK. Time evolution of the emissionmeasure of the plasma above 10 MK at the ribbons has a peak near the HXR peaktime. The presence of hot plasma in the lower atmosphere is further confirmedby RHESSI imaging spectroscopy analysis, which shows resolved sources at 11-13MK associated with at least one ribbon. We found that collisional beam heatingcan only marginally explain the necessary power to heat the 10 MK plasma at theribbons.

Impulsive Heating of Solar Flare Ribbons Above 10 MK