Achieving Fast Reconnection in Resistive MHD Models via Turbulent Means
arXiv:1110.0089 · doi:10.5194/npg-19-251-2012
Abstract
Astrophysical fluids are generally turbulent and this preexisting turbulence must be taken into account for the models of magnetic reconnection which are attepmted to be applied to astrophysical, solar or heliospheric environments. In addition, reconnection itself induces turbulence which provides an important feedback on the reconnection process. In this paper we discuss both theoretical model and numerical evidence that magnetic reconnection gets fast in the approximation of resistive MHD. We consider the relation between the Lazarian & Vishniac turbulent reconnection theory and Lapenta's numerical experiments testifying of the spontaneous onset of turbulent reconnection in systems which are initially laminar.
submitted to Nonlinear Processes in Geophysics
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Cited by in corpus (10)
- Turbulence, Magnetic Reconnection in Turbulent Fluids and Energetic Particle Acceleration
- Turbulent Reconnection and Its Implications
- Relativistic magnetic reconnection in collisionless ion-electron plasmas explored with particle-in-cell simulations
- PIC Simulation Methods for Cosmic Radiation and Plasma Instabilities
- Separatrices: the crux of reconnection
- Gamma-ray Bursts Induced by Turbulent Reconnection
- Evolution, structure and topology of self-generated turbulent reconnection layers
- Magnetic Reconnection in Astrophysical Environments
- Energy exchanges in reconnection outflows
- Theory and Applications of Non-Relativistic and Relativistic Turbulent Reconnection