Longitudinal drift of Tayler instability eigenmodes as a possible explanation for super-slowly rotating Ap stars

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Fig. 4.

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Fractional growth rate of the instability as a function of the normalised amplitude of the background field of Eq. (1). The dashed line corresponds to the diffusion parameters of Eq. (7) and the full line corresponds to the reduced thermal diffusion of ϵ_χ = 10⁻⁴.

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