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This lecture explores the properties of strong Alfvénic turbulence in magnetized relativistic collisionless plasma, a phenomenon common in astrophysical environments. Learn how this type of turbulence creates intermittent current structures at smaller scales, becomes affected by tearing instability, and serves as an effective mechanism for nonthermal particle acceleration in magnetically dominated environments. Discover the relationship between turbulent magnetic fluctuations and the guiding magnetic field, and how this impacts both the energy spectrum of accelerated particles and their pitch angle distribution—factors that potentially influence the radiative signatures of astrophysical objects. This 49-minute presentation by Stanislav Boldyrev from the Simons Foundation provides valuable insights into plasma physics and astrophysical processes.
