Several models for the winds of O stars have been proposed to explain the unexpected presence of high ionization potential ions such as N+4 and O+5. Lamers and Snow (1978) proposed that the winds of stars showing N V and O VI lines have elevated temperatures near 4±2 × 105K while cooler stars with anomalous Si IV lines have Te ≈ 7±3 × 104K. Alternately, Cassinelli and Olson (1978, CO) and Olson (1978) have explained the presence of these ions by showing that a thin corona at the base of a cool wind (Te ≲ Teff) can produce these ions by the Auger photoionization process where a single x-ray photon causes the ejection of two electrons. A third possibility is that the winds are at only slightly elevated temperatures (40 000 to 60 000K) and photoionization in an optically thick wind produces the unexpected ions. The problem of determining the local radiation field in such a wind is discussed by Klein and Castor (1978). The purpose of the present analysis is to test the ability of these three wind models to fit the observations of ζ Orionis A 09.7 Ib.