2007/12/31 by Seiji Zenitani, S. Zenitani, M. Hoshino · 8 citations
Physics and Astronomy · #Ionosphere and magnetosphere dynamics #Magnetic confinement fusion research #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.1086/528708
Astrophysical Journal, 677, 530; 35 pages, 15 figures
arxiv created 2008/03/28 · openalex publication_date 2008/04/04 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We study the role of guide field in relativistic magnetic reconnection in a Harris current sheet of pair (e ± ) plasmas, using linear theories and particlein-cell (PIC) simulations. Two-dimensional PIC simulations exhibit the guide field dependence to the linear instabilities; the tearing or reconnection modes are relatively insensitive, while the relativistic drift-kink instability (RDKI), the fastest mode in a relativistic current sheet, is stabilized by the guide field. Particle acceleration in the nonlinear stage is also investigated. A three-dimensional PIC simulation demonstrates that the current sheet is unstable to the RDKI, although small reconnection occurs in the deformed current sheet. Another threedimensional PIC simulation with a guide field demonstrates a completely different scenario. Secondary magnetic reconnection is triggered by nonlinear coupling of oblique instabilities, which we call the relativistic drift-sausage tearing instability. Therefore, particle acceleration by relativistic guide field reconnection occurs in three-dimensional configuration. Based on the plasma theories, we discuss an important role of guide field — to enable non-thermal particle acceleration by magnetic reconnection. Subject headings: acceleration of particles — magnetic fields — plasmas — instabilities — relativity 1.