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We extend the analysis of Penev et al. (2007) to calculate effectiveviscosities for the surface convective zones of three main sequence stars of0.775Msun, 0.85Msun and the present day Sun. In addition we also pay carefulattention to all normalization factors and assumptions in order to deriveactual numerical prescriptions for the effective viscosity as a function of theperiod and direction of the external shear. Our results are applicable forperiods that are too long to correspond to eddies that fall within the inertialsubrange of Kolmogorov scaling, but no larger than the convective turnovertime, when the assumptions of the calculation break down. We find linearscaling of effective viscosity with period and magnitudes at least three timeslarger than the Zahn (1966, 1989) prescription.

Dissipation Efficiency in Turbulent Convective Zones in Low Mass Stars