Formation of current sheets in magnetic reconnection

物理 当前工作表 磁重联 磁场 涡度 电流(流体) 消散 等离子体 外场线 磁流体力学 电流密度 磁能 等离子板 经典力学 机械 磁层 涡流 磁化 量子力学 热力学
作者
Allen H. Boozer
出处
期刊:Physics of Plasmas [American Institute of Physics]
卷期号:21 (7) 被引量:16
标识
DOI:10.1063/1.4890491
摘要

An ideal evolution of magnetic fields in three spatial dimensions tends to cause neighboring field lines to increase their separation exponentially with distance ℓ along the lines, δ(ℓ)=δ(0)eσ(ℓ). The non-ideal effects required to break magnetic field line connections scale as e−σ, so the breaking of connections is inevitable for σ sufficiently large—even though the current density need nowhere be large. When the changes in field line connections occur rapidly compared to an Alfvén transit time, the constancy of j||/B along the magnetic field required for a force-free equilibrium is broken in the region where the change occurs, and an Alfvénic relaxation of j||/B occurs. Independent of the original spatial distribution of j||/B, the evolution is into a sheet current, which is stretched by a factor eσ in width and contracted by a factor eσ in thickness with the current density j|| increasing as eσ. The dissipation of these sheet currents and their associated vorticity sheets appears to be the mechanism for transferring energy from a reconnecting magnetic field to a plasma. Harris sheets, which are used in models of magnetic reconnection, are shown to break up in the direction of current flow when they have a finite width and are in a plasma in force equilibrium. The dependence of the longterm nature of magnetic reconnection in systems driven by footpoint motion can be studied in a model that allows qualitative variation in the nature of that motion: slow or fast motion compared to the Alfvén transit time and the neighboring footpoints either exponentially separating in time or not.
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