Modeling the Solar Dynamo.

The article discusses how numerical simulations are changing astronomers' views on the dynamo process underlying the solar magnetic activity cycle. Topics include the evolution of the Sun's magnetic field, an overview of dynamos, which are self-sustained amplifications of magnetic fields through the action of fluid motions, and the impact of parallel advances in raw computing and numerical algorithms on the ability of astronomers to produce and investigate magnetic cycles in Sun-like spheres with a thermally convecting magnetized fluid. A discussion of magnetohydrodynamics (MHD) and three images of a magnetohydrodynamical numerical simulation of solar convection via the multiscale flow simulation model EULAG are presented.