Turbulence properties and associated particle transport in 3D low-beta magnetic reconnection

Reconnection-generated turbulence plays a crucial role in particle acceleration and transport in the reconnection region. Using 3D kinetic simulations of magnetic reconnection, we investigate the characteristics of this turbulence and the associated particle transport. Our study focuses on the weak guide-field regime relevant to the Earth's magnetotail and solar flares, where particle acceleration is highly efficient. By analyzing cross-scale energy transfer with scale-filtering techniques, we observe that a substantial portion of the released magnetic energy cascades from large to small scales, resembling a turbulence cascade. The turbulence properties, including the turbulence spectrum and anisotropy scaling in the reconnection region, are broadly consistent with current turbulence theory. Tracing the magnetic field lines reveals that neighboring lines can separate exponentially, indicating a superdiffusion process. Particles moving along these lines also exhibit superdiffusion while simultaneously experiencing scattering by turbulence fluctuations, resulting in a mixing of superdiffusion and normal diffusion. Using test-particle simulations, we evaluate the spatial transport coefficients in such turbulence reconnection regions. These findings are essential for understanding high-energy particle acceleration in magnetic reconnection and have significant implications for fundamental reconnection and turbulence physics in space and astrophysical plasmas.