Ideal kink instability of a magnetic loop equilibrium

Details Ideal kink instability of a magnetic loop equilibrium Ideal kink instability of a magnetic loop equilibrium

2003-11-09

arxiv.org/abs/astro-ph/0311198v1

Astron.Astrophys. 413 (2004) L27

Astronomy and Astrophysics

Astrophysics

Astron. Astrophys. Lett., accepted

Scientific paper

10.1051/0004-6361:20031691

The force-free coronal loop model by Titov & D\'emoulin (1999} is found to be unstable with respect to the ideal kink mode, which suggests this instability as a mechanism for the initiation of flares. The long-wavelength ($m=1$) mode grows for average twists $\Phi\ga3.5\pi$ (at a loop aspect ratio of $\approx$ 5). The threshold of instability increases with increasing major loop radius, primarily because the aspect ratio then also increases. Numerically obtained equilibria at subcritical twist are very close to the approximate analytical equilibrium; they do not show indications of sigmoidal shape. The growth of kink perturbations is eventually slowed down by the surrounding potential field, which varies only slowly with radius in the model. With this field a global eruption is not obtained in the ideal MHD limit. Kink perturbations with a rising loop apex lead to the formation of a vertical current sheet below the apex, which does not occur in the cylindrical approximation.

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