Parametric Study of Current Sheets and Vorticity Sheets in Relativistic Turbulence

Turbulence is widely believed to play a critical role in particle heating and acceleration across a broad range of astrophysical environments. These include the solar corona and Earth's magnetosphere, as well as highly magnetized systems where magnetic energy exceeds plasma internal energy, leading to relativistic turbulence, such as jets from active galactic nuclei (AGN) and gamma-ray bursts (GRBs). In this study, we employ particle-in-cell (PIC) simulations to investigate how current sheets depend on plasma magnetization (σ) and the relative strength of magnetic fluctuations (δB/B₀). Using a self-organizing map (SOM) algorithm, we systematically identify current sheets and associated reconnection sites within the turbulent plasma. Our statistical analysis quantifies the distribution of current sheet properties, including length, width, and thickness, and examines how these properties scale with magnetization and fluctuation amplitude. We perform an analogous analysis for vorticity sheets, allowing us to study how turbulence organizes the spatial distribution of reconnection sites and regions of high vorticity. This dual characterization of current and vorticity sheet structures across parameter space provides key diagnostics for understanding how turbulence mediates magnetic reconnection in relativistic plasmas. This systematic analysis of sheet structure and dynamics may inform the development of particle acceleration theories that more accurately incorporate injection processes, anisotropic effects, nonthermal acceleration mechanisms, and the spatial localization of acceleration sites in turbulent, reconnecting systems.