Volume 514, May 2010
|Number of page(s)||14|
|Published online||06 May 2010|
Reconnection in weakly stochastic B-fields in 2D
Astronomical Observatory, Jagiellonian
University, ul Orla 171, 30-244 Kraków, Poland e-mail: firstname.lastname@example.org
2 Department of Astronomy, University of Wisconsin, 475 North Charter Street, Madison, WI 53706, USA
3 Department of Physics and Astronomy, McMaster University, 1280 Main Street West, Hamilton, ON L8S 4M1, Canada
Accepted: 5 January 2010
We study two-dimensional turbulent magnetic reconnection in a compressible fluid in the gas pressure dominated limit. We use open boundary conditions and start from a Harris current sheet configuration with a uniform total pressure. A small perturbation of the vector potential initiates laminar reconnection at the Sweet-Parker rate, which is allowed to evolve for several dynamical times. Subsequently sub-Alfvenic turbulence is produced through random forcing at small wave numbers. The magnetic field topology near the current sheet is strongly affected by the turbulence. However, we find that the resulting reconnection speed depends on the resistivity. In contrast to previous results in three dimensions, we find no evidence for fast reconnection. The reconnection speed exhibits strong variations, but the time averages increase smoothly with the strength of the turbulence.
Key words: galaxies: magnetic fields / turbulence / magnetohydrodynamics (MHD)
© ESO, 2010
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