Abstract
It is proposed that the formation of the morphology of solar magnetic cavities and of the topology of their magnetic fields at a certain stage of their evolution (a decay of a quasi-uniform, rotating, magnetized cylindrical layer into rings, followed by their deformation and the generation of internal fine structure etc.) can be attributed to the excitation of a shear-centrifugal-resonance instability. The calculations show the existence of two families of unstable modes: resonance-gyroscopic modes due to the rotation of the layer and fast magneto acoustic waves propagating outside the layer and resonating in phase with intra-layer perturbations. Both families contain a large number of unstable waveguide harmonics, with the superposition and interaction of these harmonics being responsible for the extremely complex structure of coronal cavities.
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Original Russian Text © R.A. Bisengaliev, V.V. Mustsevoi, A.A. Solov’ev, 2014, published in Astronomicheskii Zhurnal, 2014, Vol. 91, No. 4, pp. 308–319.
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Bisengaliev, R.A., Mustsevoi, V.V. & Solov’ev, A.A. Centrifugal effects and the Kelvin-Helmholtz instability in coronal cavities. Astron. Rep. 58, 249–259 (2014). https://doi.org/10.1134/S1063772914040027
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DOI: https://doi.org/10.1134/S1063772914040027