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Fig. A.4

image

Typical power spectra of velocity (black lines) and magnetic field (red lines) from the middle of the convective layer for Code 1 (left), Code 2 (middle), and Code 3 (right). In each case, the inset shows the smallest wavenumbers to illustrate that the magnetic field peaks at k = 0. All spectra quantities are normalised by the average kinetic energy at zm during the non-linear phase.

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