  Recent observations of the spectral line profiles and intensity ratio of the
O VI 1032 {\AA} and 1037.6 {\AA} doublet by the Ultraviolet Coronagraph
Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO), made in
coronal holes below 3.5 $R_s$, provide evidence for Doppler dimming of the O VI
1037.6 {\AA} line and pumping by the chromospheric C II 1037.0182 {\AA} line.
Evidence for a significant kinetic temperature anisotropy of O$^{5+}$ ions was
also derived from these observations. We show in this Letter how the component
of the kinetic temperature in the direction perpendicular to the magnetic
field, for both isotropic and anisotropic temperature distributions, affects
both the amount of Doppler dimming and pumping. Taking this component into
account, we further show that the observation that the O VI doublet intensity
ratio is less than unity can be accounted for only if pumping by C II 1036.3367
{\AA} in addition to C II 1037.0182 {\AA} is in effect. The inclusion of the C
II 1036.3367 {\AA} pumping implies that the speed of the O$^{5+}$ ions can
reach 400 km/s around 3 $R_s$ which is significantly higher than the reported
UVCS values for atomic hydrogen in polar coronal holes. These results imply
that oxygen ions flow much faster than protons at that heliocentric distance.
