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The solar-stellar experiment started with the HK Project at Mount Wilson Observatory initiated by Olin Wilson in 1966, continued with the hunt for solar analogs up through the eighties and nighties and have culminated so-far with the remarkable results from CoRoT and Kepler.  \section{Introduction}  With the term \textit{the solar-stellar connection} we understand primary the field where studies of Sun-like stars are used to increase our understanding of the Sun. In this review we will focus on how Sun-like stars can be used to increased our understanding of the solar dynamo. The solar dynamo can theoretical be described by the magnetohydrodynamical (MHD) induction equation: equation\cite{2005LRSP....2....2C}:  \begin{equation}  \frac{\partial {\rm \bf B}}{\partial t} = \nabla \times \left({\rm \bf u} \times {\rm \bf B} - \eta \nabla \times {\rm \bf B} \right) 
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{\rm \bf u} = {\rm \bf u_p}\left( r,\theta \right) + r ~{\rm sin}~\theta ~ \Omega \left( r, \theta \right) \hat {\rm e}_{\phi}  \end{equation}  This field includes a great variety where $r$ is the distance from the center  of different subjects, but the Sun and $\Omaga$ is the angular velocity.   It is thus clear that in order  for this review we have make the Sun or other Sun-like stars to host  a selective of what we think are dynamo they need to have magnetic fields, differential rotation and meridional circulation or convection. These ingredience have thus been chosen as  the most important subjects: subject to be covered by this review:  \begin{itemize}  \item Magnetic fields