Confinement of the Solar Tachocline by Dynamo Action in the Radiative Interior

A major outstanding problem in solar physics is the confinement of tachocline, thin shear layer that separates nearly solid-body rotation radiative interior from strong differential convection zone. Here, we present first 3-D, global simulation which a tachocline confined by self-excited dynamo. The non-axisymmetric magnetism initially built zone and then diffusively imprints downward. Additionally, field locally amplified throughout vigorous horizontal motions arise equatorial Rossby waves possibly instabilities. Our work thus challenges long-held notion Sun's dynamo magnetic only as deep stored quiescent interior.