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Fig. C.2.


Power spectra for m = 1. Top row: power for the four components , , , and . The purple contours delineate the regions where inflows into active regions produce excess power (see Fig. C.1). The two blue curves show m(Ω − ΩCarr)/2π at the surface and at r = 0.95 R. Second row: power spectral density averaged over 0° −30°. The gray curves show the power spectra at full resolution (3.06 nHz), and the black curves show them at a quarter of the resolution. The 95% confidence levels are shown by the red horizontal lines. The cyan curves are for the quiet-Sun period only (2.6 years from 4 February 2018 to 6 September 2020). Third row: power spectral density averaged over 15° −45°. Fourth row: power spectral density averaged over 37.5° −67.5°. In the three lower rows, the dots and the shaded areas (see legend) indicate the significant peaks and the excess power ranges not related to magnetic activity, given in Table A.1.

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