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On Kelvin–Helmholtz and parametric instabilities driven by coronal waves

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Figure

Figure 1. Panel (a): a large-scale schematic diagram of an oscillating flux tube rooted in the solar photosphere
Figure 2. Calculation of the variation of η′ with T for MA = 0.2, and α+ = 0.01 using θ = 1.48 (where θ = tan −1(Ky/Kx)) in panels (a) and (c), θ = 1.20 inpanel (b), θ = 1.45 in panel (d), θ = 1.5 in panel (e), and θ = 1.45 in panel (f)
Figure 3. Numerically computed logarithm of the growth rate in0.2. The labelled blue arrows show the position inletters A–D mark different instability bands, where Adashed line marks the critical wavenumber for the growth of the KH instability in the asymp
Figure 4. Numerically computed logarithm of the growth rate in K-space for (a) α+ = 1/11 and MA = 0.02 and (b) α+ = 2/5 and MA = 0.02

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