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Turbulent properties of the quiet Sun represent the basic state of surfaceconditions, and a background for various processes of solar activity. Thereforeunderstanding of properties and dynamics of this `basic' state is important forinvestigation of more complex phenomena, formation and development of observedphenomena in the photosphere and atmosphere. For characterization of theturbulent properties we compare kinetic energy spectra on granular andsub-granular scales obtained from infrared TiO observations with the New SolarTelescope (Big Bear Solar Observatory) and from 3D radiative MHD numericalsimulations ('SolarBox' code). We find that the numerical simulations require ahigh spatial resolution with 10 - 25 km grid-step in order to reproduce theinertial (Kolmogorov) turbulence range. The observational data require anaveraging procedure to remove noise and potential instrumental artifacts. Theresulting kinetic energy spectra show a good agreement between the simulationsand observations, opening new perspectives for detailed joint analysis of morecomplex turbulent phenomena on the Sun, and possibly on other stars. Inaddition, using the simulations and observations we investigate effects ofbackground magnetic field, which is concentrated in self-organized complicatedstructures in intergranular lanes, and find an increase of the small-scaleturbulence energy and its decrease at larger scales due to magnetic fieldeffects.

Turbulent Kinetic Energy Spectra of Solar Convection from NST Observations and Realistic MHD Simulations