Abstract

When our Sun was younger it rotated much more rapidly. Observations of many young stars indicate that magnetic activity and perhaps dynamo action are stronger in the rapidly rotating suns. Here we use the anelastic spherical harmonic (ASH) code to explore 3-D MHD simulations of the dynamo action ... Show moreWhen our Sun was younger it rotated much more rapidly. Observations of many young stars indicate that magnetic activity and perhaps dynamo action are stronger in the rapidly rotating suns. Here we use the anelastic spherical harmonic (ASH) code to explore 3-D MHD simulations of the dynamo action that might occur in such younger suns. As a great surprise, we find that coherent global-scale structures of toroidal magnetic field are formed in the bulk of the convection zone. These wreaths of magnetism persist for long periods of time amidst the still turbulent convection. In contrast to previous solar dynamo simulations, the wreaths of magnetism formed in these more rapidly rotating suns do not require a tachocline of penetration and shear at the base of the convection zone for their creation or survival. Show less