Institution(s): 1. Lockheed Martin Solar and Astrophysics Laboratory
Surface flux transport models have proven useful for modeling the evolution of magnetic patterns on the solar photospheric surface on timescales ranging from as short as a few days to as long as multiple magnetic cycles. In the work presented here, we use surface flux transport models to study variations in the magnetic activity of Sun-like stars, and to explore the dependence of flux evolution on the properties of flux emergence, large-scale flows, and dispersal by convective turbulence. These time sequences of surface magnetic evolution are then used to drive magnetofrictional models of stellar coronal fields to study how coronal fields evolve. From such models, we can begin to assess how the evolution of various stellar features, such as interacting starspot groups, might affect the overlying stellar coronae.