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Please note the unusual time (3pm PDT) due to time-zone difficulty.

The solar differential rotation (DR) is one of the fundamental properties of the Sun, but its origin and maintenance are not fully understood. In our recent studies (Hotta & Kusano, 2021; Hotta et al., 2022), we demonstrated that the presence of strong magnetic fields is a key ingredient for constructing solar-like DR, and it may provide a possible solution to the long-standing convective conundrum. Subsequent investigations have further supported this scenario, in particular through (1) the near-surface shear layer and (2) DR in slowly rotating stars. In addition, we have confirmed the robustness of these results by (3) demonstrating numerical convergence in global convection simulations.

In this presentation, we will review these findings and discuss their implications for our understanding of solar and stellar interior dynamics.