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The idea behind the B{\"o}hm-Vitense diagram was taken up by \cite{Karoff_2009} and \cite{Karoff_2013} in their {\it sounding stellar cycles with Kepler} project, who rely on the fact the asteroseismic observations from the {\it Kepler} mission could be used to test the hypothesis that the discontinuous break between for stars around the age of the Sun is caused by a change in the dynamo action which she suggest is due to abruptly increased deep mixing. This is possible as asteroseismology can be used to measure both ages, differential rotation and ages of the stars. Unfortunally, {\it Kepler} was only fully operational for four years, which appears to be to short to allow any firm detection of stellar cycles using {\it Kepler} observations alone. The project does however continue using ground-based facilities to measure activity cycles.  \cite{Garcia_2010} was the first to realize that the high precision space photometry could be used to search for stellar cycles. They reported the detection of a stellar activity cycle with a period of at least 120 days. This is however much shorted than any of the activity cycles detected in the observations from the Mount Wilson and Lowel observatories. Though it might be immature to call the signal in HD 49933 detected by CoRoT a cycle, the reason why the possible cycle period might be so sort could be that this star is an F type star with a very thin outer convection zone. This is supported by a number of other studies, including