Magnetic stochasticity is shown to be quantitatively tied to the diffusion law of the field, with simulation data favoring the super-linear Richardson scaling.
Inertial-Range Reconnection in Magnetohydrodynamic Turbulence and in the Solar Wind
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abstract
In situ spacecraft data on the solar wind show events identified as magnetic reconnection with outflows and apparent "`$X$-lines" $10^{3-4}$ times ion scales. To understand the role of turbulence at these scales, we make a case study of an inertial-range reconnection event in a magnetohydrodynamic (MHD) simulation. We observe stochastic wandering of field-lines in space, breakdown of standard magnetic flux-freezing due to Richardson dispersion, and a broadened reconnection zone containing many current sheets. The coarse-grain magnetic geometry is like large-scale reconnection in the solar wind, however, with a hyperbolic flux-tube or "$X$-line" extending over integral length-scales.
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Magnetic stochasticity and diffusion
Magnetic stochasticity is shown to be quantitatively tied to the diffusion law of the field, with simulation data favoring the super-linear Richardson scaling.