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\citet{2003ApJ...586..464B, 2007ApJ...669.1167B} combined these studies into the term he call {\it gyrochronology} -- i.e. how to relate stellar rotation periods to stellar ages. The idea is that FGKM stars separate into three different sequences: the I sequence, the C sequence and the R sequence. I stand for {\it interface} and represents stars that have a coupling between the radiative interior and the convective envelope. C stands for {\it convective} and represents stars with deep convective zones, where the radiative interior is decoupled from the convective envelope and where a $\alpha\Omega$ and an $\alpha^2\Omega$ dynamo have not yet set in. R stands for {\it radiative} and represents early F-type stars with very thin convective zones that are thus dominated by the radiative interior. A note of caution here. The I, C and R sequences by \citet{2003ApJ...586..464B} have nothing to do with the active and inactive branches by \cite{1998ApJ...498L..51B}. Stars on both the active and the inactive branch are likely to have an $\alpha\Omega$ or an $\alpha^2\Omega$ dynamo, where as stars on the C sequence are likely to have an $\alpha^2$ dynamo. Though dynamos in the stars on the R sequence are likely to be $\alpha^2\Omega$ dynamos (ref), they are also likely to have a rather different nature than the dynamos on the I sequence. The stars on the I sequence, however, can belong both to the active and the inactive branch.  The first study of rotation periods in a large ensemble of stars using {\it Kepler} observations was done by \cite{2011A&A...529A..89D} who identified 3200 stars that show signs of rotational modulation and of activity in the light curve, using a supervised classifier on a number of Fourier parameters of the light curves. \cite{2012A&A...539A.137M, 2013MNRAS.432.1203M, 2013ApJ...775L..11M,2014ApJS..211...24M} have done a series of studies of rotation modulation of {\it Kepler light} curves.  [figure]  results from CoRot and Kepler