ON THE IMPORTANCE OF HIGH-M INSTABILITIES IN LINE-TIED CORONAL MAGNETIC-FIELDS

It is shown that for the determination of the magnetohydrodynamical (M HD) stability of coronal magnetic fields, where the photospheric line- tying effect is a basic element of the physical description, it is imp ortant to consider modes of both low and high angular wave number m. I n particular, when the equilibrium deviates from the force-free state, modes with high m may have higher growth rates than the m = 1 (kink) mode. It is then possible that high-m modes become unstable when the f ield line length increases in the evolution of the equilibrium, while the m = 1 mode remains stable. This is important because the high-m mo des intrinsically lead to strong dissipation. This contrasts to the ca se of the one-dimensional infinite (i.e. not line-tied) cylinder, wher e it is sufficient to prove stability of the m = 1 mode to guarantee s tability for all modes m > 1 (Newcomb 1960). In the line-tied case how ever, there exists no prior reason to only consider m = 1 instabilitie s in coronal magnetic fields.