Speaker
Description
Understanding plasma turbulence in curved spacetime — especially near compact objects — remains an open challenge. Conventional analyses rely on flat-spacetime techniques that cannot fully capture the effects of strong gravitational curvature. In this work, we review a recent method for studying turbulence in generic manifolds and arbitrary gravitational fields, enabling the calculation of quantities such as the second-order structure function and power spectral density in a fully relativistic framework. Finally, we apply this method to numerical simulations of accretion on a Kerr black hole, showing that such curvature-based approach reproduces the expected inertial-range cascade while uncovering significant discrepancies with flat-spacetime analyses close to the black hole event horizon.
