| Issue |
A&A
Volume 516, June-July 2010
|
|
|---|---|---|
| Article Number | A5 | |
| Number of page(s) | 9 | |
| Section | The Sun | |
| DOI | https://doi.org/10.1051/0004-6361/201014041 | |
| Published online | 16 June 2010 | |
Dynamics of braided coronal loops
I. Onset of magnetic reconnection
Division of Mathematics, University of Dundee, Dundee, DD1 4HN, UK e-mail: antonia@maths.dundee.ac.uk
Received:
11
January
2010
Accepted:
2
April
2010
Aims. The response of the solar coronal magnetic field to small-scale photospheric boundary motions including the possible formation of current sheets via the Parker scenario is one of open questions of solar physics. Here we address the problem via a numerical simulation.
Methods. The three-dimensional evolution of a braided magnetic field which is initially close to a force-free state is followed using a resistive MHD code.
Results. A long-wavelength instability takes place and leads to the formation of two thin current layers. Magnetic reconnection occurs across the current sheets with three-dimensional features shown, including an elliptic magnetic field structure about the reconnection site, and results in an untwisting of the global field structure.
Key words: magnetohydrodynamics (MHD) / plasmas / Sun: corona / magnetic fields
© ESO, 2010
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