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.
Highlights
Astrophysical plasmas are known to be magnetized and turbulent
Apart from showing non-thermal Doppler broadening, spectra of supersonic turbulent velocity fluctuations have been revealed when analyzed with techniques like Velocity Channel Analysis (VCA) or Velocity Coordinate Spectrum (VCS) developed and applied to the observational data rather recently
Fast turbulent reconnection is critically linked with selffeeding flow patterns and with the feedback by turbulence induced by the outflow on the reconnection process
Summary
Astrophysical plasmas are known to be magnetized and turbulent. Turbulence is really ubiquitous in most astrophysical environments. It is important to understand the process of magnetic reconnection in a realistically turbulent state of the fluid. It is important to understand the mutual feedback of turbulence and reconnection and provide the connection between the existing theory, observations and numerical experiments. This is the goal of the present paper. We discuss magnetic reconnection in turbulent fluid, provide the numerical confirmations of the predictions of the LV99 model, consider the spontaneous onset of reconnection in MHD simulations, and the role of flow pattern in Sect.
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