On the MHD stability of the M=1 kink mode in finite length coronal loops

Details On the MHD stability of the M=1 kink mode in finite length coronal loops On the MHD stability of the M=1 kink mode in finite length coronal loops

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.285..105v&link_type=abstract

In ESA, Proceedings of an International School and Workshop on Reconnection in Space Plasma, Volume 2 p 105-109 (SEE N89-24974 1

Computer Science

Coronal Loops, Magnetohydrodynamic Stability, Solar Magnetic Field, Equations Of Motion, Fourier Series, Lines Of Force, Plasma Conductivity

Scientific paper

A general method for studying the ideal and resistive MHD stability of plasma configurations with line-tying is presented, and applied to the case of the M=1 kink mode in coronal loops. The method consists in a truncated Fourier series approach applied to the linearized equations of motion, and is found to converge rapidly with the order of the truncation. Models of the boundary conditions at the corona-photosphere interface are discussed, and the growth rates of unstable modes are calculated for equilibrium profiles with an without a reversal in the field component connecting to the photosphere. The relevance of these modes to compact loop flares is assessed.

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