Inertial-Range Reconnection in Magnetohydrodynamic Turbulence and in the Solar Wind

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.