  The Discrete Absorption Components (DACs) commonly observed in the
ultraviolet lines of hot stars have previously been modelled by dynamical
simulations of Corotating Interaction Regions (CIRs) in their line-driven
stellar winds. Here we apply the kinematic DAC inversion method of Brown et al.
to the hydrodynamical CIR models and test the reliability of the results
obtained. We conclude that the inversion method is able to recover valuable
information on the velocity structure of the mean wind and to trace movement of
velocity plateaux in the hydrodynamical data, though the recovered density
profile of the stream is correct only very near to the stellar surface.
