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• W3103487675 endingPage "263" @default.
• W3103487675 startingPage "251" @default.
• W3103487675 abstract "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." @default.
• W3103487675 created "2020-11-23" @default.
• W3103487675 creator A5028300061 @default.
• W3103487675 creator A5065740298 @default.
• W3103487675 date "2012-04-03" @default.
• W3103487675 modified "2023-10-16" @default.
• W3103487675 title "Achieving fast reconnection in resistive MHD models via turbulent means" @default.
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• W3103487675 doi "https://doi.org/10.5194/npg-19-251-2012" @default.
• W3103487675 hasPublicationYear "2012" @default.
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