An Analytical Model of the Kelvin-Helmholtz Instability of Transverse Coronal Loop Oscillations

Abstract

Recent numerical simulations have demonstrated that transverse coronal loop oscillations are susceptible to the Kelvin-Helmholtz (KH) instability due to the counter-streaming motions at the loop boundary. We present the first analytical model of this phenomenon. The region at the loop boundary where the shearing motions are greatest is treated as a straight interface separating time-periodic counter-streaming flows. In order to consider a twisted tube, the magnetic field at one side of the interface is inclined. We show that the evolution of the displacement at the interface is governed by Mathieu's equation and we use this equation to study the stability of the interface. We prove that the interface is always unstable, and that, under certain conditions, the magnetic shear may reduce the instability growth rate. The result, that the magnetic shear cannot stabilise the interface, explains the numerically found fact that the magnetic twist does not prevent the onset of the KH instability at the boundary of an oscillating magnetic tube. We also introduce the notion of the loop $\sigma$-stability. We say that a transversally oscillating loop is $\sigma$-stable if the KH instability growth time is larger than the damping time of the kink oscillation. We show that even relatively weakly twisted loops are $\sigma$-stable.

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• Identification of Nonlinear Damping of Transverse Loop Oscillations by KHI-induced Turbulence
• Magnetic reconnection and the Kelvin-Helmholtz instability in the solar corona