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Magnetized turbulence and magnetic reconnection are often invoked to explainthe nonthermal emission observed from a wide variety of astrophysical sources.By means of fully-kinetic 2D and 3D PIC simulations, we investigate theinterplay between turbulence and reconnection in generating nonthermalparticles in magnetically-dominated pair plasmas. A generic by-product of theturbulence evolution is the generation of a nonthermal particle spectrum with apower-law energy range. The power-law slope $p$ is harder for largermagnetizations and stronger turbulence fluctuations, and it can be as hard as$p < 2$. The Larmor radius of particles at the high-energy cutoff is comparableto the size $l$ of the largest eddies. Plasmoid-mediated reconnection, whichself-consistently occurs in the turbulent plasma, controls the physics ofparticle injection. Then, particles are further accelerated by stochasticscattering off turbulent fluctuations. The work done by parallel electricfields - naturally expected in reconnection layers - is responsible for most ofthe initial energy increase, and is proportional to the magnetization $\sigma$of the system, while the subsequent energy gain, which dominates the overallenergization of high-energy particles, is powered by the perpendicular electricfields of turbulent fluctuations. The two-stage acceleration process leaves animprint in the particle pitch-angle distribution: low-energy particles arealigned with the field, while the highest energy particles move preferentiallyorthogonal to it. The energy diffusion coefficient of stochastic accelerationscales as $D_\gamma\sim 0.1\sigma(c/l)\gamma^2$, where $\gamma$ is the particleLorentz factor. This results in fast acceleration timescales $t_{acc}\sim(3/\sigma)\,l/c$. Our findings have important implications for understandingthe generation of nonthermal particles in high-energy astrophysical sources.

The interplay of magnetically-dominated turbulence and magnetic reconnection in producing nonthermal particles