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Turbulent mixing of chemical elements by convection has fundamental effectson the evolution of stars. The standard algorithm at present, mixing-lengththeory (MLT), is intrinsically local, and must be supplemented by extensionswith adjustable parameters. As a step toward reducing this arbitrariness, wecompare asteroseismically inferred internal structures of two Kepler slowlypulsating B stars (SPB's; $M\sim 3.25 M_\odot$) to predictions of 321Dturbulence theory, based upon well-resolved, truly turbulent three-dimensionalsimulations (Arnett , et al. 2015, Christini, et al. 2016) which includeboundary physics absent from MLT. We find promising agreement between thesteepness and shapes of the theoretically-predicted composition profile outsidethe convective region in 3D simulations and in asteroseismically constrainedcomposition profiles in the best 1D models of the two SPBs. The structure andmotion of the boundary layer, and the generation of waves, are discussed.

Synergies between Asteroseismology and Three-dimensional Simulations of Stellar Turbulence