On the MHD stability of the vec m = 1 kink mode in solar coronal loops

Details On the MHD stability of the vec m = 1 kink mode in solar coronal loops On the MHD stability of the vec m = 1 kink mode in solar coronal loops

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...367..321b&link_type=abstract

Astronomy and Astrophysics, v.367, p.321-325 (2001)

Astronomy and Astrophysics

Astrophysics

23

Sun: Corona, Mhd, Methods: Numerical, Instabilities

Scientific paper

We revisit the ideal MHD stability of the m = 1 kink mode in configurations representative of coronal loops, using a stability code. We adopt different magnetic force-free equilibria defined by the twist function that are embedded into an outer potential field situated at a radial distance r_0 from the magnetic axis. In the limit r_0 >> l_0, l_0 being the axis pitch length, the configurations are driven unstable by the kink mode when the twist exceeds the classical critical value of 2.5 pi on the axis. However, the critical axis twist strongly depends on the equilibrium in the opposite limit, with sharply increasing values when r_0 becomes of the order or smaller than l_0. We interpret these results in terms of the stability criterion _l = 2.5 pi , where _l is the twist value averaged over a radial length l. It is found that l is of the order of 3-4 times l_0, provided r_0/l_0 >~ 5; otherwise it depends on the twist profile via the existence of magnetic resonances.

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