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