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Fig. 5.


Top: predicted difference in the Rossby mode frequencies between the two solar maxima (grey curve, 2014 minus 2002) and between the maximum of cycle 24 and the preceding solar minimum (brown curve, 2014 minus 2009). The error bars are propagated errors from the scatter in the solar rotation measurements. Bottom: estimated errors in the Rossby mode frequencies due to the finite mode lifetimes as a function of observation time T. These errors can be used to determine whether the predicted frequency shifts from the top panel are detectable.

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