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We present results from particle-in-cell simulations of driven turbulence inmagnetized, collisionless, and relativistic pair plasma. We find thatfluctuations are consistent with the classical $k_\perp^{-5/3}$ magnetic energyspectrum at fluid scales and a steeper $k_\perp^{-4}$ spectrum at sub-Larmorscales, where $k_\perp$ is the wavevector perpendicular to the mean field. Wedemonstrate the development of a non-thermal, power-law particle energydistribution, $f(E) \sim E^{-\alpha}$, with index $\alpha$ that decreases withincreasing magnetization and increases with increasing system size (relative tothe characteristic Larmor radius). Our simulations indicate that turbulence canbe a viable source of energetic particles in high-energy astrophysical systems,such as pulsar wind nebulae, if scalings asymptotically become insensitive tothe system size.

Kinetic turbulence in relativistic plasma: from thermal bath to non-thermal continuum