Self-generated turbulence in magnetic reconnection

Abstract

Classical Sweet-Parker models of reconnection predict that reconnection rates depend inversely on the resistivity, usually parameterized using the dimensionless Lundquist number ($\Lund$). We describe magnetohydrodynamic (MHD) simulations using a static, nested grid that show the development of a three-dimensional instability in the plane of a current sheet between reversing field lines without a guide field. The instability leads to rapid reconnection of magnetic field lines at a rate independent of $\Lund$ over at least the range $3.2\times 10^3 \lesssim \Lund \lesssim 3.2 \times 10^5$ resolved by the simulations. We find that this instability occurs even for cases with $\Lund \lesssim 10^4$ that in our models appear stable to the recently described, two-dimensional, plasmoid instability. Our results suggest that three-dimensional, MHD processes alone produce fast (resistivity independent) reconnection without recourse to kinetic effects or external turbulence. The unstable reconnection layers provide a self-consistent environment in which the extensively studied turbulent reconnection process can occur.

5 pages; 4 figures. Accepted to ApJL

References in corpus (4)

• Instability of current sheets and formation of plasmoid chains
• Numerical Tests of Fast Reconnection in Weakly Stochastic Magnetic Fields
• On the role of fast magnetic reconnection in accreting black hole sources
• A magnetic reconnection model for explaining the multi-wavelength emission of the microquasars Cyg X-1 and Cyg X-3

Cited by in corpus (15)

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• Damping of Alfven waves by Turbulence and its Consequences: from Cosmic-Rays Streaming to Launching Winds
• Flux ropes and dynamics of the heliospheric current sheet
• Ponderomotive Acceleration in Coronal Loops
• MHD simulations of three-dimensional Resistive Reconnection in a cylindrical plasma column
• Formation and Reconnection of Three-dimensional Current Sheets with a Guide Field in the Solar Corona
• Comparative statistics of selected subgrid-scale models in large eddy simulations of decaying, supersonic MHD turbulence
• Forced magnetic reconnection and plasmoid coalescence: I - MHD Simulations
• Evolution, structure and topology of self-generated turbulent reconnection layers
• Stochastic Turbulent Acceleration in a fractal environment
• Activation of MHD reconnection on ideal timescales
• Filamentary plasma eruptions and the heating and acceleration of electrons