Electron acceleration in interaction of helical magnetic structure in three-dimensional large temporal-spatial turbulent magnetic reconnection

Solar flare, as a typical large temporal-spatial turbulent magnetic reconnection (LTSTMR, the ratio of observed current sheets thickness to electron characteristic length, electron Larmor radius for low-β and electron inertial length for high-β, is on the order of 10E10–10E11; the ratio of observed evolution time to electron gyroperiod is on the order of 10E7–10E9) explosion in the solar atmosphere activities, involving sudden bursts of particle acceleration that from sudden release of magnetic energy in a few minutes to a few tens of minutes. The X rays and gamma rays are believed to result from the interactions of the high energy electrons energized and nuclear interaction of the high energy protons and other heavier ions, respectively. While many particle acceleration models consider turbulence acceleration as an effective way of generating energetic electrons, the precise turbulence roles during acceleration and heating of electrons still remain unclear. Here we show from 3D relativistic hybrid partic...