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We assess the global-scale dynamo action achieved in a simulation of asun-like star rotating at three times the solar rate. The 3-D MHD AnelasticSpherical Harmonic code, using slope-limited diffusion, is employed to captureconvection and dynamo processes in such a young sun. The simulation is carriedout in a spherical shell that encompasses 3.8 density scale heights of thesolar convection zone. We find that dynamo action with a high degree of timevariation occurs, with many periodic polarity reversals every 6.2 years. Themagnetic energy also rises and falls with a regular period, with two magneticenergy cycles required to complete a polarity cycle. These magnetic energycycles arise from a Lorentz-force feedback on the differential rotation,whereas the polarity reversals are present due to the spatial separation of theequatorial and polar dynamos. Moreover, an equatorial migration of toroidalfield is found, which is linked to the changing differential rotation and to anear-surface shear layer. This simulation also enters a grand minimum lastingroughly 20 years, after which the dynamo recovers its regular polarity cycles.

Cycling Dynamo in a Young Sun: Grand Minima and Equatorward Propagation