Magnetic reconnection with anomalous resistivity in two-and-a-half dimensions I: Quasi-stationary case
arXiv:astro-ph/0508094 · doi:10.1063/1.2084847
Abstract
In this paper quasi-stationary, two-and-a-half-dimensional magnetic reconnection is studied in the framework of incompressible resistive magnetohydrodynamics (MHD). A new theoretical approach for calculation of the reconnection rate is presented. This approach is based on local analytical derivations in a thin reconnection layer, and it is applicable to the case when resistivity is anomalous and is an arbitrary function of the electric current and the spatial coordinates. It is found that a quasi-stationary reconnection rate is fully determined by a particular functional form of the anomalous resistivity and by the local configuration of the magnetic field just outside the reconnection layer. It is also found that in the special case of constant resistivity reconnection is Sweet-Parker and not Petschek.
15 pages, 4 figures, minor changes as compared to the 1st version
Cited by in corpus (17)
- Instability of current sheets and formation of plasmoid chains
- A Reconnection Switch to Trigger Gamma-Ray Burst Jet Dissipation
- Physical Origin of the Quadrupole Out-of-Plane Magnetic Field in Hall-MHD Reconnection
- Turbulent Magnetic Reconnection in Two Dimensions
- Stellar Explosions by Magnetic Towers
- Plasmoid and Kelvin-Helmholtz instabilities in Sweet-Parker current sheets
- Fast Collisionless Reconnection Condition and Self-Organization of Solar Coronal Heating
- Magnetically-dominated jets inside collapsing stars as a model for gamma-ray bursts and supernova explosions
- Self-Regulation of Solar Coronal Heating Process via Collisionless Reconnection Condition
- A model of Hall reconnection
- An iterative semi-implicit scheme with robust damping
- Model of two-fluid reconnection
- On Flux Rope Stability and Atmospheric Stratification in Models of Coronal Mass Ejections Triggered by Flux Emergence
- An evaluation of possible mechanisms for anomalous resistivity in the solar corona
- Fast Magnetic Reconnection induced by Resistivity Gradients in 2D Magnetohydrodynamics
- On the two-dimensional magnetic reconnection with nonuniform resistivity
- Fast and slow two-fluid magnetic reconnection