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A number studies have also searched and found indication of stellar cycles in stars later than F. \cite{2015A&A...583A.134F} tried to measure rotation periods in 16 FGK main-sequence stars using observations from CoRoT. Periods between 33 and 650 days are found. Though simulations predict that only half of these cycle period should be true, it is remarkable to see the nice relation between rotation and cycle period, including the identification of a active and an inactive branch. \cite{2015ApJS..221...18H} analyzed to G-type stars, with rotation periods of 6.0 and 14.7 days and found indication of activity cycles of 1.3 and 2.5 years respectively. Again, this is shorter than the periods found by \cite{Baliunas_1995} and here both studies are looking at Sun-like stars. By comparing the photometric variability observed in these two stars with the Sun, \cite{2015ApJS..221...18H} arrives at another very interesting conclusion, i.e. that the rotational modulations of the light curves observed by {\it Kepler} for these two stars are caused by bright faculae and not dark spots.  A number of studies have been published analyzing photometric variability in {\it Kepler} light curves \cite{2011AJ....141...20B} \cite{2010ApJ...713L.155B} \cite{2011AJ....141...50W}, \cite{2013MNRAS.436.1883W}, \cite{2015arXiv151203454B}, \cite{2014ApJ...788L...9B}, \cite{2013Natur.500..427B}, without attributing this variability to stellar cycles. We will come back to these studies in the next sections.