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 particle-in-cell and lattice Boltzmann method (RHPIC-LBM) simulation that interaction of helical magnetic structure that leads to efficient energization of electrons. By following the trajectories of the most energetic electrons, we found the strong Langmuir turbulence acceleration (LTA) through wave-wave, wave-particle interaction in the diffusion region of the flare, which can accelerate electrons effectively. and discuss the turbulence acceleration by strong Langmuir wave. The simulation of LTA is not only similar to the shock wave acceleration, but more efficient than that of the shock wave acceleration. The energy spectrum of hot electrons undergoing LTA can be studied the X ray and gamma ray production in flare. We anticipate our results to be a key point for understanding the relationship between particle acceleration mechanism and explosive energetic electrons observed in the solar flares during MHD Alfven turbulence translate into Kinetic Alfven turbulence progress.