  An update is given on the current status of solar and stellar dynamos. At
present, it is still unclear why stellar cycle frequencies increase with
rotation frequency in such a way that their ratio increases with stellar
activity. The small-scale dynamo is expected to operate in spite of a small
value of the magnetic Prandtl number in stars. Whether or not the global
magnetic activity in stars is a shallow or deeply rooted phenomenon is another
open question. Progress in demonstrating the presence and importance of
magnetic helicity fluxes in dynamos is briefly reviewed, and finally the role
of nonlocality is emphasized in modeling stellar dynamos using the mean-field
approach. On the other hand, direct numerical simulations have now come to the
point where the models show solar-like equatorward migration that can be
compared with observations and that need to be understood theoretically.
