Helioseismology and asteroseismology are both advancing rapidly, each inspired by the observational tools that have either become available recently, or will soon be functioning. Thus GONG+, SOHO/MDI, MOST and soon CoRoT and SDO/HMI will each contribute to expanding the data bases available for probing the interior of stars, joined by a range of individual observational projects. Although variable stars come in many forms, the sun and solar-like stars share many aspects that challenge our understanding of the interior dynamics and structure attained within them. The intricate coupling of turbulent convection, rotation and magnetism plays a central role in these stars, and much of this can now be probed, especially with spatially-resolved observations of the sun. Thus the Rubik's Cube has many elements, both from local helioseismic probing and from theoretical modeling, that are likely to become aligned as we rotate the panels and attain a clearer picture of what occurs within a star. We discuss some of the dynamical issues that are likely to be a focus of new observational and analysis efforts now under way and being planned. The structure of the solar near-surface shear layer with its multiple scales of motion, many interacting with magnetism, is beginning to be intensely studied. Yet its dynamic origin and potential variability as the solar cycle advances has yet to be clarified. The manner in which the solar differential rotation appears to be established within the bulk of the convection zone is now partly understood through simulations, placing significant constraints on the patterns of meridional circulations that are likely present. Since these are more complex than assumed in mean field flux-transport models that replicate some aspects of the solar cycle, it is essential to get guidance from helioseismic deductions about the deeper circulations. The tachocline of rotational shear at the base of the convection zone is the likely seat of the global dynamo, providing the means to build strong toroidal magnetic fields that eventually erupt. Devising helioseismic means to probe variations in this region should be a major effort as we try to devise and test self-consistent dynamical models for this subtle boundary layer. The sun continues to reveal itself as a remarkably complex magnetic star, a property likely shared by many other stars now being studied or contemplated.
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