Achieving fast reconnection in resistive MHD models via turbulent means

15Citations
Citations of this article
7Readers
Mendeley users who have this article in their library.

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. © Author(s) 2012. CC Attribution 3.0 License.

Cite

CITATION STYLE

APA

Lapenta, G., & Lazarian, A. (2012). Achieving fast reconnection in resistive MHD models via turbulent means. Nonlinear Processes in Geophysics, 19(2), 251–263. https://doi.org/10.5194/npg-19-251-2012

Register to see more suggestions

Mendeley helps you to discover research relevant for your work.

Already have an account?

Save time finding and organizing research with Mendeley

Sign up for free