Achieving Fast Reconnection in Resistive MHD Models via Turbulent Means

TL;DR

This paper explores how turbulence influences magnetic reconnection in resistive MHD, demonstrating that turbulence can induce fast reconnection rates through theoretical models and numerical experiments.

Contribution

It links turbulent reconnection theory with numerical evidence showing spontaneous fast reconnection in initially laminar systems.

Findings

Turbulence accelerates magnetic reconnection in resistive MHD.

Numerical experiments confirm spontaneous onset of turbulent reconnection.

Theoretical models align with simulation results.

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.