Recorded 31 January 2025. Loren Matilsky of the University of California, Santa Cruz, presents "The solar dynamo may confine the tachocline and cause rigid shellular rotation at all depths" at IPAM's Rotating Turbulence: Interplay and Separability of Bulk and Boundary Dynamics Workshop. Abstract: In the solar interior, strong latitudinal differential rotation persists throughout most of the convection zone (CZ). At the base of the CZ, this differential rotation transitions across a narrow shear layer, known as the "tachocline", to rigid rotation in the radiative zone (RZ) below. This rigidity persists as far down as seismology can reliably probe. The origin of the tachocline and rigid rotation of the RZ both remain mysteries, given the known tendency of shear to radiatively spread inward very quickly. We explore three-dimensional magnetohydrodynamic simulations of a solar-like CZ-RZ system, in which the nonaxisymmetric magnetic field from a quasi-periodic convective dynamo spreads into the RZ via a new type of skin effect. This field causes a Maxwell stress which forces the RZ into rigid rotation and confines a tachocline against radiative spread. Furthermore, the steady-state angular momentum profiles in our magnetic simulations indicate that the CZ (as a whole) rotates very slightly faster than the RZ, a fact which remarkably appears to be true for the seismically observed Sun as well. We speculate that the solar dynamo field, via its skin effect, could connect all depths of the Sun and force the whole system to have a nearly constant shellular rotation rate. Learn more online at: https://www.ipam.ucla.edu/programs/workshops/rotating-turbulence-interplay-and-separability-of-bulk-and-boundary-dynamics/