Journal
NONLINEAR PROCESSES IN GEOPHYSICS
Volume 19, Issue 2, Pages 251-263Publisher
COPERNICUS GESELLSCHAFT MBH
DOI: 10.5194/npg-19-251-2012
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Funding
- NSF [AST 0808118]
- Center for Magnetic Self Organization in Laboratory and Astrophysical Plasmas (CMSO)
- NASA MMS mission
- KU Leuven
- European Commission [218816, 263340]
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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.
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