  The current understanding of the turbulent dissipation in stellar convective
zones is based on the assumption that the turbulence follows Kolmogorov
scaling. This assumption is valid for some cases in which the time frequency of
the external shear is high (e.g., solar p modes). However, for many cases of
astrophysical interest (e.g., binary orbits, stellar pulsations, etc.), the
timescales of interest lie outside the regime of applicability of Kolmogorov
scaling. We present direct calculations of the dissipation efficiency of the
turbulent convective flow in this regime, using simulations of anelastic
convection with external forcing. We show that the effects of the turbulent
flow are well represented by an effective viscosity coefficient, we provide the
values of the effective viscosity as a function of the perturbation frequency
and compare our results to the perturbative method for finding the effective
viscosity of Penev et al. that can be applied to actual simulations of the
surface convective zones of stars.
