Dynamics of braided coronal loops

Issue		A&A Volume 516, June-July 2010


Article Number		A5
Number of page(s)		9
Section		The Sun
DOI		10.1051/0004-6361/201014041
Published online		16 June 2010

A&A 516, A5 (2010)

I. Onset of magnetic reconnection

A. L. Wilmot-Smith, D. I. Pontin and G. Hornig

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

Abstract

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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