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Fig. 5.


Comparison of our cycle period measurements to results from (a) Baliunas et al. (1995), (b) Saikia et al. (2018), (c) Olspert et al. (2018), and (d) Messina & Guinan (2002). The open circle indicates the star HD 201092 for which only a chromospheric cycle period was measured. Crosses indicate secondary periods connected by vertical dotted lines to the primary periods. The dashed line shows the 1:1 identity, and the dotted lines to either side mark the ±20% range. We set the cycle period to zero for stars in common for which no cycle period was reported.

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