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The goal of this research is to investigate how well various turbulencemodels can describe physical properties of the upper convective boundary layerof the Sun. An accurate modeling of the turbulence motions is necessary forunderstanding the excitation mechanisms of solar oscillation modes. We havecarried out realistic numerical simulations using several different physicalLarge Eddy Simulation (LES) models (Hyperviscosity approach, Smagorinsky, anddynamic models) to investigate how the differences in turbulence modelingaffect the damping and excitation of the oscillations and their spectralproperties and compare with observations. We have first calculated theoscillation power spectra of radial and non-radial modes supported by thecomputational box with the different turbulence models. Then we have calculatedthe work integral input to the modes to estimate the influence of theturbulence model on the depth and strength of the oscillation sources. We havecompared these results with previous studies and with the observed propertiesof solar oscillations. We find that the dynamic turbulence model provides thebest agreement with the helioseismic observations.

Numerical simulation of excitation of solar oscillation modes for different turbulent models