Dynamics of braided coronal loops. I. Onset of magnetic reconnection
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.
- Publication:
-
Astronomy and Astrophysics
- Pub Date:
- June 2010
- DOI:
- 10.1051/0004-6361/201014041
- arXiv:
- arXiv:1001.1717
- Bibcode:
- 2010A&A...516A...5W
- Keywords:
-
- magnetohydrodynamics (MHD);
- plasmas;
- Sun: corona;
- magnetic fields;
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 18 pages, 9 figures