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Fig. C.7.
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Stream functions Ψ(θ, ϕ, t = 0) for the m = 1, 2, and 3 Rossby modes R, R1, and R2, some of which may be unstable. The differential rotation is that of the Sun’s surface (temporal average) and the Ekman number is E = 2 × 10−4. The red curves show the latitudes of the viscous critical layers.
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