  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.
