Articles | Volume 19, issue 2
Nonlin. Processes Geophys., 19, 251–263, 2012
https://doi.org/10.5194/npg-19-251-2012

Special issue: Magnetic reconnection and turbulence in space, laboratory...

Nonlin. Processes Geophys., 19, 251–263, 2012
https://doi.org/10.5194/npg-19-251-2012

Review article 03 Apr 2012

Review article | 03 Apr 2012

Achieving fast reconnection in resistive MHD models via turbulent means

G. Lapenta1 and A. Lazarian2 G. Lapenta and A. Lazarian
  • 1Centrum voor Plasma-Astrofysica, Departement Wiskunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
  • 2Department of Astronomy, University of Wisconsin-Madison, 475 Charter St., USA

Abstract. Astrophysical fluids are generally turbulent and this preexisting turbulence must be taken into account for models of magnetic reconnection in 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 the theoretical model and numerical evidence that magnetic reconnection becomes fast in the approximation of resistive MHD. We consider the relation between the Lazarian and Vishniac turbulent reconnection theory and Lapenta's numerical experiments testifying of the spontaneous onset of turbulent reconnection in systems which are initially laminar.