  The development of 2D and 3D simulations of solar convection has lead to a
picture of convection quite unlike the usually assumed Kolmogorov spectrum
turbulent flow. We investigate the impact of this changed structure on the
dissipation properties of the convection zone, parametrized by an effective
viscosity coefficient. We use an expansion treatment developed by Goodman & Oh
1997, applied to a numerical model of solar convection (Robinson et al. 2003)
to calculate an effective viscosity as a function of frequency and compare this
to currently existing prescriptions based on the assumption of Kolmogorov
turbulence (Zahn 1966, Goldreich & Keeley 1977). The results match quite
closely a linear scaling with period, even though this same formalism applied
to a Kolmogorov spectrum of eddies gives a scaling with power-law index of 5/3.
