Rotational effects in turbulence driven by convection

We have treated turbulence with rotation in a thin Keplerian disk. Highlighting implicit assumptions already existent in the alpha model together with a geometrical but physically reasonable deduction of the degrees of freedom of the largest eddies, which is of paramount importance in our formulation, we were able to obtain relations satisfied by parameters of the turbulence, such as turnover time and alpha. The effects of rotation in the turbulence we have taken implictly through an anisotropy factor (x) which is simply related to the Rossby number. Convection is the process assumed to generate turbulence, and we have used Canuto and Goldman's treatment of convective instability, whose characteristic growth time we have assumed equal to the turnover time. We have also used their procedure to obtain the turbulent viscosity.