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Abstract
Stars can be fascinating settings in which to study intricate couplings among convection, rotation, magnetism, and shear, usually under distinctly nonlinear conditions that yield vigorous turbulence. The emerging flux and the rotation rates of stars can vary widely, yet there are common elements that must contribute to building and maintaining the vibrantly evolving magnetic activity they exhibit. Some of these elements, such as the rotational shear and meridional flows established by the coupling of convection with rotation, can now be studied in detail within our nearest star using helioseismology. Major three-dimensional numerical simulations help refine our intuitions about such interior dynamics, aided by rapid advances in supercomputing that are improving the fidelity of the modeling. These developments, combined with intense thrusts at new high resolution and continuous observations of solar magnetism and solar oscillations, herald a promising era for exploring such astrophysical fluid dynamics.