Space climate and weather is driven by magnetic fields generated by a dynamo below the surface of the Sun and other stars. In the recent years there have been great advances in modelling solar and stellar dynamos using mean-field models as well as 3D global convection models. However, the problem remains how to quantify turbulent dynamo effects important for the magnetic field evolution. One way to tackle this problem is to parametrize them from theories of turbulence, another way is to deduced them from solar observation and a third way is the measure them from global convective dynamo simulations for example with the test-field method. This talk will review these three ways and how their outcome impacts our understanding of solar and stellar dynamo. Furthermore, I will discuss how stellar observation will further help us in constraining our theories of solar and stellar dynamos driving space climate.