A comparison between modelled O* intensities and V1 observations, shown as a function of radial distance. The V1 energetic O intensities are averaged over 0.10-AU-wide intervals and plotted against radial distance for five energy ranges (as shown). Statistical uncertainties are not shown, but are below approximately 10% (smaller than the symbol size) after the TS crossing and 50% (comparable to the symbol size) immediately upstream. For some energies both the modelled and observed intensities are multipled by scaling factors for clarity, as indicated in the legend. The position of the TS is indictated by the vertical line. The model results are shown at a polar angle of 55° for the qA  <  0 magnetic polarity cycle, as is appropriate for the corresponding observations. The vertical dashed line shows the approximate position (at r = 120 AU) where non-radial solar wind flow may begin to dominate.