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Particle acceleration is one of the most significant features that areubiquitous among space and cosmic plasmas. It is most prominent during flaresin the case of the Sun, with which huge amount of electromagnetic radiation andhigh-energy particles are expelled into the interplanetary space throughacceleration of plasma particles in the corona. Though it has been wellunderstood that energies of flares are supplied by the mechanism calledmagnetic reconnection based on the observations in X-rays and EUV with spacetelescopes, where and how in the flaring magnetic field plasmas are acceleratedhas remained unknown due to the low plasma density in the flaring corona. Wehere report the first observational identification of the energetic non-thermalelectrons around the point of the ongoing magnetic reconnection (X-point); withthe location of the X-point identified by soft X-ray imagery and the localizedpresence of non-thermal electrons identified from imaging-spectroscopic data attwo microwave frequencies. Considering the existence of the reconnectionoutflows that carries both plasma particles and magnetic fields out from theX-point, our identified non-thermal microwave emissions around the X-pointindicate that the electrons are accelerated around the reconnection X-point.Additionally, the plasma around the X-point was also thermally heated up to 10MK. The estimated reconnection rate of this event is ~0.017.

Evidence of Electron Acceleration around the Reconnection X-point in a Solar Flare