  We discuss how recent advances in observations, theory and numerical
simulations have allowed the stellar community to progress in its understanding
of stellar convection, rotation and magnetism and to assess the degree to which
the Sun and other stars share similar dynamical properties. Ensemble
asteroseismology has become a reality with the advent of large time domain
studies, especially from space missions. This new capability has provided
improved constraints on stellar rotation and activity, over and above that
obtained via traditional techniques such as spectropolarimetry or CaII H&K
observations. New data and surveys covering large mass and age ranges have
provided a wide parameter space to confront theories of stellar magnetism.
These new empirical databases are complemented by theoretical advances and
improved multi-D simulations of stellar dynamos. We trace these pathways
through which a lucid and more detailed picture of magnetohydrodynamics of
solar-like stars is beginning to emerge and discuss future prospects.
