We have constructed models for the sun at three stages of its evolution: a zero-age main sequence model, the present sun, and a subgiant model. For each model, the turbulent pressure and turbulent kinetic energy were calculated from 3-d radiative hydrodynamical simulations (described in the poster by Robinson et al.), and inserted into the 1-d stellar models. We note that in these simulations, the turbulent pressure is not a free parameter, but can be computed from the resulting velocity field. We show the calculated p-mode frequencies for the model of the present sun, with and without turbulent pressure, and compare them to the observed solar frequencies. When the turbulent pressure is included in the models, the calculated frequencies are brought closer to the observed frequencies in the sun by up to two $mu Hz$, strictly from structural effects. The effect of including turbulent pressure on p-mode frequencies is also shown for the zero-age main sequence model. Our models also suggest that the importance of turbulent pressure increases as the star evolves into the subgiant region. We discuss the importance of also including realistic turbulence as well as radiation in the non-adiabatic calculation of oscillation frequencies.
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