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The paradigm change to to a very small radial differential rotation in the convection zone had a huge impact on our understanding of the solar dynamo. Here the idea of a so-called $\alpha \Omega$ dynamo {\it distributed} of the convection zone had to be abandoned \cite{2005LRSP....2....2C}. Instead a so called {\it interface} dynamo was proposed, where the $\alpha$ effect is seated at the tachocline was more accepted, but this subjected has attached renewed attention in recent years, partly do to new observations of {\it slower} rotating cores in red giants. Mean-field dynamo models of the solar are most often so-called $\alpha \Omega$ dynamos, where the the toroidal component of the magnetic field is driven by rotational shear (the $\Omega$ effect) and the poloidal component is driven by turbulence (the $\alpha$ effect). For fully convective M stars the dynamo responsible for generating the magnetic field is expected to be a so-called $\alpha^2$ dynamo, where the $\alpha$ effect is driving both the toroidal and the polodial component of the magnetic field (ref). In young stars with week differential rotation the dynamo could be a so-called $\alpha^2\Omega$ dynamo, where the toroidal component of the magnetic field is driven by both the $\alpha$ and the $\Omega$ (as discussed for the F-type stars \cite{2013ApJ...777..153A}). The existing of this zoo of dynamo models suggest that the nature of the solar dynamo might not has been as it is now, throughout the whole life of the Sun and that we should be carefully with assuming that we understanding the dynamo in the Sun.   THe theoretical description of how stars loss angular momentum to stellar winds was formulated by \cite{1984LNP...193...49M} and tested on stellar models by \cite{1988ApJ...333..236K}. This analysis suggested that though stars are form with a verity of different initial angular momentum, but the time the stars reach an age of 80 million years, then have also spun so much down that their rotation rate is independent of the initial angular momentum. This explains the strong relation between rotation rate and age seen by \cite{Skumanich_1972}, but the general picture is still that the angular momentum is distributed evenly over the convection zones of the stars. This was changes with the model by \cite{1990ApJS...74..501P} who used a set of coupled diffusion equations to describe the internal transport of angular momentum throughout the convection zone. These calculation show that F and G type stars losses angular momentum more efficient than K and M type stars. As the F and G type stars have thiner convective zone and larger radiative zones than K and M stars, F and G type stars will build up a stronger tachocline. THis will lead to a coupling between the radiative interior and the outer convection zone. In the K and M type stars there will be no such coupling and the angular momentum can therefore only be lost from the (thick) convective zone, which will lead to a relative faster spin-down rate.  \cite{2003ApJ...586..464B} combined these studies into the term he call {\it gyrochronology}.  Recently,   \section{Convection}