Magnetism in Global Solar and Stellar Dynamos
Ben Brown

Our Sun is a magnetic star, and magnetism is a ubiquitous feature of other sun-like stars. The magnetic fields that we observe at the surface, and the magnetic activity that heats the chromosphere and corona, are driven by dynamo processes in the sub-surface solar convection zone. Here I will talk about recent advances in global-scale 3-D MHD simulations of stellar dynamos. Convection and large-scale flows couple to build wreath-like global-scale magnetic structures in the convection zone. The polarity of these magnetic fields can cyclically reverse with cycle periods of several years. These simulations are now being connected with spectropolarimetric Zeeman Doppler imaging observations of global-scale stellar magnetic fields. I will also discuss emerging puzzles about solar convection, advances in our understanding of the low-mach number fluid equations that we use in studying deep solar and stellar convection, and the path forward with such global-scale simulations.