WKB estimates for the onset of ideal MHD instabilities in solar coronal loops

Details WKB estimates for the onset of ideal MHD instabilities in solar coronal loops WKB estimates for the onset of ideal MHD instabilities in solar coronal loops

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..150...99h&link_type=abstract

Solar Physics, vol. 150, no. 1-2, p. 99-115

Physics

Plasma Physics

8

Applications Of Mathematics, Coronal Loops, Force-Free Magnetic Fields, Magnetohydrodynamic Stability, Mathematical Models, Photosphere, Plasma Equilibrium, Solar Magnetic Field, Solar Prominences, Wentzel-Kramer-Brillouin Method, Boundary Conditions, Differential Equations, Eigenvalues, Eigenvectors, Fourier Analysis, Fourier Series, Lagrangian Function, Magnetic Field Configurations, Plasma Physics

Scientific paper

A Wentzel-Kramer-Brillouin (WKB) approach, based on the method of Connor, Hastie, and Taylor (1979), is used to obtain simple estimates of the critical conditions for the onset of ideal magnetohydrodynamic (MHD) instabilities in line-tied solar coronal loops. The method is illustrated for the constant twist, Gold-Hoyle (1960) field, and the critical conditions are compared with previous and new numerical results. For the force-free case, the WKB estimate for the critical loop length reduces to (2 * pi * m) + (pi * square root of 2). For the sufficiently non-force-free case the critical length can be expressed in the form (l0 + l1)/m. The results confirm the findings of De Bruyne and Hood (1992) that for force-free fields the m = 1 mode is the first mode to become unstable but for the sufficiently strong non-force-free case this reverses with the m approaches infinity mode being excited first.

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