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Stars like the Sun are formed from rotating molecular cloud. As these cloud contract, they will stars to spin-up, in order to conserve angular momentum. This means that Sun-like stars, as they arrive on the main-sequence, will be rotating relatively fast. Naively, we would assume that Sun-like stars would have close to homogenous rotation when they arrive on the main sequence, but even this assumption is like not corrects (ref). We would then expect that the star spin-down through out the convection zone and thus build up radial differential rotation in the convection zone. This is how ever also not correct. This was proven from the first helioseismic observations of progrande and retrograde sectroal oscillations modes by \citet{1984Natur.310...19D, 1985Natur.317..591B}. These observations revealed that the solar convection zone rotated at more or less the same rotation profile as the solar surface leaving all the radial shear to the thin border between the radiation and the convection zone. A region that have later been names the {\it tachocline} \citep{1992A&A...265..106S}. \citet{1998ApJ...505..390S} used observations from the Michelson Doppler Imager (MDI) on the Solar and Heliospheric Observatory (SOHO) spacecraft to calculate was should properly be names the standard to rotation profile. This profile shows that the decrease in angular velocity with increasing latitude seen on the surface continues all the way down to the tachocline, where a strong shear layer change the latitudinal rotation profile of the convection zone to a solid body rotation rotation in the radiation zone.   The paradime 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 $\aplha \Omega$ dynamo distributed {\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 $\aplha \Omega$ 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 $\lapha^2\Omega$ dynamo, where the toroidal component of the magnetic field is driven by both the $\alpha$ and the $\Omega$ (as discussed for the T-type stars).  Recently,