{ "id": "2108.13940", "version": "v1", "published": "2021-08-31T15:59:44.000Z", "updated": "2021-08-31T15:59:44.000Z", "title": "Kinetic Simulations of Imbalanced Turbulence in a Relativistic Plasma", "authors": [ "Amelia Hankla", "Vladimir Zhdankin", "Gregory Werner", "Dmitri Uzdensky", "Mitchell Begelman" ], "comment": "Submitted to MNRAS", "categories": [ "astro-ph.HE", "physics.plasm-ph", "physics.space-ph" ], "abstract": "Turbulent high-energy astrophysical systems often feature asymmetric energy injection or driving: for instance, nonlinear interactions between Alfv\\'en waves propagating from an accretion disk into its corona. Such systems -- relativistic analogs of the solar wind -- are \"imbalanced\": the energy fluxes parallel and anti-parallel to the large-scale magnetic field are unequal and the plasma therefore possesses net cross-helicity. In the past, numerical studies of imbalanced turbulence have focused on the magnetohydrodynamic regime. In the present study, we investigate externally-driven imbalanced turbulence in a collisionless, ultrarelativistically hot, magnetized pair plasma using three-dimensional particle-in-cell simulations. We find that a turbulent cascade forms for every value of imbalance covered by the simulations and that injected Poynting flux efficiently converts into net momentum of the plasma, a relativistic effect with implications for the launching of a disk wind. Surprisingly, particle acceleration remains efficient even for very imbalanced turbulence. These results characterize properties of imbalanced turbulence in a collisionless plasma and have ramifications for black hole accretion disk coronae, winds, and jets.", "revisions": [ { "version": "v1", "updated": "2021-08-31T15:59:44.000Z" } ], "analyses": { "keywords": [ "imbalanced turbulence", "kinetic simulations", "relativistic plasma", "poynting flux efficiently converts", "black hole accretion disk coronae" ], "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable" } } }