2013/01/31 by Yi-Min Huang, A. Bhattacharjee · 3 citations
Physics and Astronomy · #Ionosphere and magnetosphere dynamics #Magnetic confinement fusion research #Solar and Space Plasma Dynamics #astro-ph.SR #physics.geo-ph #physics.plasm-ph #physics.space-ph
paper · pdf · doi:10.1063/1.4802941
published as Phys. Plasmas 20, 055702 (2013) · Revision submitted to Phys. Plasmas, references added
arxiv created 2013/02/08 · openalex publication_date 2013/04/29 · arxiv updated 2013/05/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Our understanding of magnetic reconnection in resistive magnetohydrodynamics has gone through a fundamental change in recent years. The conventional wisdom is that magnetic reconnection mediated by resistivity is slow in laminar high Lundquist (S) plasmas, constrained by the scaling of the reconnection rate predicted by Sweet-Parker theory. However, recent studies have shown that when S exceeds a critical value ∼104, the Sweet-Parker current sheet is unstable to a super-Alfvénic plasmoid instability, with a linear growth rate that scales as S1/4. In the fully developed statistical steady state of two-dimensional resistive magnetohydrodynamic simulations, the normalized average reconnection rate is approximately 0.01, nearly independent of S, and the distribution function f(ψ) of plasmoid magnetic flux ψ follows a power law f(ψ)∼ψ−1. When Hall effects are included, the plasmoid instability may trigger onset of Hall reconnection even when the conventional criterion for onset is not satisfied. The rich variety of possible reconnection dynamics is organized in the framework of a phase diagram.