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We conduct a wide-band X-ray spectral analysis in the energy range of 1.5-100keV to study the time evolution of the M7.6 class flare of 2016 July 23, withthe Miniature X-ray Solar Spectrometer (MinXSS) CubeSat and the Reuven RamatyHigh Energy Solar Spectroscopic Imager (RHESSI) spacecraft. With thecombination of MinXSS for soft X-rays and RHESSI for hard X-rays, a non-thermalcomponent and three-temperature multi-thermal component -- "cool" ($T \approx$3 MK), "hot" ($T \approx$ 15 MK), and "super-hot" ($T \approx$ 30 MK) -- weremeasured simultaneously. In addition, we successfully obtained the spectralevolution of the multi-thermal and non-thermal components with a 10 s cadence,which corresponds to the Alfv\'en time scale in the solar corona. We find thatthe emission measures of the cool and hot thermal components are drasticallyincreasing more than hundreds of times and the super-hot thermal component isgradually appearing after the peak of the non-thermal emission. We also studythe microwave spectra obtained by the Nobeyama Radio Polarimeters (NoRP), andwe find that there is continuous gyro-synchrotron emission from mildlyrelativistic non-thermal electrons. In addition, we conducted a differentialemission measure (DEM) analysis by using Atmospheric Imaging Assembly (AIA)onboard the Solar Dynamics Observatory (SDO) and determine that the DEM of coolplasma increases within the flaring loop. We find that the cool and hot plasmacomponents are associated with chromospheric evaporation. The super-hot plasmacomponent could be explained by the thermalization of the non-thermal electronstrapped in the flaring loop.

Study of Time Evolution of Thermal and Non-Thermal Emission from an M-Class Solar Flare