  The goal of this research is to investigate how well various turbulence
models can describe physical properties of the upper convective boundary layer
of the Sun. An accurate modeling of the turbulence motions is necessary for
understanding the excitation mechanisms of solar oscillation modes. We have
carried out realistic numerical simulations using several different physical
Large Eddy Simulation (LES) models (Hyperviscosity approach, Smagorinsky, and
dynamic models) to investigate how the differences in turbulence modeling
affect the damping and excitation of the oscillations and their spectral
properties and compare with observations. We have first calculated the
oscillation power spectra of radial and non-radial modes supported by the
computational box with the different turbulence models. Then we have calculated
the work integral input to the modes to estimate the influence of the
turbulence model on the depth and strength of the oscillation sources. We have
compared these results with previous studies and with the observed properties
of solar oscillations. We find that the dynamic turbulence model provides the
best agreement with the helioseismic observations.
