Title: Synergies between Asteroseismology and Three-dimensional Simulations of Stellar Turbulence,
Abstract: Turbulent mixing of chemical elements by convection has fundamental effects
on the evolution of stars. The standard algorithm at present, mixing-length
theory (MLT), is intrinsically local, and must be supplemented by extensions
with adjustable parameters. As a step toward reducing this arbitrariness, we
compare asteroseismically inferred internal structures of two Kepler slowly
pulsating B stars (SPB's; $M\sim 3.25 M_\odot$) to predictions of 321D
turbulence theory, based upon well-resolved, truly turbulent three-dimensional
simulations (Arnett , et al. 2015, Christini, et al. 2016) which include
boundary physics absent from MLT. We find promising agreement between the
steepness and shapes of the theoretically-predicted composition profile outside
the convective region in 3D simulations and in asteroseismically constrained
composition profiles in the best 1D models of the two SPBs. The structure and
motion of the boundary layer, and the generation of waves, are discussed.