In this talk, I will discuss work, currently in progress, aimed at modelling average properties of flows in a sub-Alfvenic regime. We focus on the transport of fluctuation energies, their associated length scale, and temperatures. We derive the model for the flows using a procedure that has been successfully applied to modelling turbulence in the solar wind from 0.3 AU on out. However, modelling the sub-Alfvenic flows within the corona presents new and different challenges, including the role of gradients in the Alfven speed and the (likely) lack of a strong turbulent cascade. These issues will be discussed and incorporated into the model. Overall, the model emphasizes relatively basic physics but provides promising beginning results.