Achieving Fast Reconnection in Resistive MHD Models via Turbulent Means

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 environ-ments. 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 rela-tion between the Lazarian & Vishniac turbulent reconnec-tion theory and Lapenta’s numerical experiments testifying of the spontaneous onset of turbulent reconnection in sys-tems which are initially laminar