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We present a self-consistent empirical model for several plasma parameters of a polar coronal hole near solar minimum, derived from observations with the Solar and Heliospheric Observatory Ultraviolet Coronagraph Spectrometer. The model describes the radial distribution of density for electrons, H , and O and the outflow of O are also significantly larger than the corresponding velocities of H . We discuss the constraints and 5ϩ 0 implications on various theoretical models of coronal heating and acceleration.

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Recent observations of the spectral line profiles and intensity ratio of the O vi ll1032 and 1037.6 doublet by the Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO), made in coronal holes below 3.5 , provide evidence for Doppler dimming of the O vi l1037.6 line and pumping R S by the chromospheric C ii l1037.0182 line. Evidence for a significant kinetic temperature anisotropy of O 5ϩ 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 of the O vi doublet intensity ratio less than unity can be accounted for only if pumping by C ii l1036.3367 in addition to C ii l1037.0182 is in effect. The inclusion of the C ii l1036.3367 pumping implies that the speed of the O 5ϩ ions can reach 400 km s Ϫ1 around 3 , which is significantly higher than the R S 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.

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