Relativistic microturbulent flares can be present in many astrophysical plasmas found e.g., in accretion disk coronae, pulsar wind nebulae, and gamma-ray bursts. In a diluted, magnetically-dominated plasma, an ensemble of these flares can produce a constant transfer of energy from large-scale bulk/shear motions into thermal and non-thermal particles. In a presence of a strong radiation field, the kinetic turbulent cascade is modified due to radiation drag experienced by the particles. The radiation alters the dynamics of the particle acceleration and in the extreme case even the turbulent cascade itself. In my presentation, I'll discuss our recent large-scale supercomputer simulations of these turbulent flares and their physics.
