  In stellar interiors shear flows play an important role in many physical
processes. So far helioseismology provides only large-scale measurements, and
so the small-scale dynamics remains insufficiently understood. To draw a
connection between observations and three-dimensional DNS of shear driven
turbulence, we investigate horizontally averaged profiles of the numerically
obtained mean state. We focus here on just one of the possible methods that can
maintain a shear flow, namely the average relaxation method. We show that
although some systems saturate by restoring linear marginal stability this is
not a general trend. Finally, we discuss the reason that the results are more
complex than expected.
