The stability of coronal loops - Finite-length and pressure-profile limits

Details The stability of coronal loops - Finite-length and pressure-profile limits The stability of coronal loops - Finite-length and pressure-profile limits

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...88..163e&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 88, Oct. 1983, p. 163-177. Research supported by the Consiglio Nazionale delle Ricerche and

Physics

81

Coronal Loops, Magnetohydrodynamic Stability, Photosphere, Pressure Gradients, Solar Corona, Astronomical Models, Boundary Value Problems, Force-Free Magnetic Fields, Solar Physics

Scientific paper

Results are described from a quickly converging, necessary-and-sufficient, MHD-stability test for coronal-loop models. The primary stabilizing influence arises from magnetic line tying at the photosphere, and this end conditions requires a series expansion of possible loop excitations. The stability boundary is shown to quickly approach a limit as the number of terms increases, providing a critical length for the loop in proportion to its transverse magnetic scale. Several models of force-free-field profiles are tested and the stability behavior of a localized current channel, embedded in an external current-free region, is shown to be superior to that of other, broader, current profiles. Pressure-gradient effects, leading to increased or decreased stability, are shown to be amplified by line tying. Long loops must either conduct low net current, or exhibit an axial-field reversal coexisting with a low-pressure core. The limits on stability depend on the magnetic aspect ratio, the plasma-to-magnetic pressure ratio, and the field orientation at the loop edge. Applications of these results to the structure of coronal loops are described.

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