The disk-wind model suggests that the broad emission lines of a quasar are emitted from the surface of the accretion disk feeding the central black hole. In this paper, we assume that a line-driven wind emerges from the illuminated face of the disk and calculate the line emission produced by this wind. The location and mass-loss rate of the wind are determined by the physics of the line driving. We calculate line ratios and the radius at which each line forms using a photoionization code. From

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... he source functions, together with simple windÈradiative transfer calculations, we then calculate line proÐles. The model reproduces the observed line ratios with a degree of success comparable to standard "" cloud ÏÏ models, underpredicting the Ñux in low-ionization lines and in N V j1240. Using C IV to Ðx all the model parameters except for the line ratios, we Ðnd that the model successfully predicts the variety of line proÐles seen in two PG quasars. We also present line proÐles for Ne VIII that are very broad (FWHM D 17,000 km s~1) and predict that Mg X, while unlikely to be seen in emission, will be seen in absorption (in broad absorption line quasars). As suggested by previous authors, we Ðnd that the very broad feature seen around j2800 and usually attributed to Mg II is actually a blend of that line, which is relatively narrow, and Fe II emission.