All Figures

$\begin{figure} \par\includegraphics[angle=90,width=7.7cm,clip]{6639fig1.eps} \end{figure}$ Figure 1: Variation of line strength indices for the UV resonance doublets of N V, Si IV, and C IV with phase in the spectrum of $\zeta$ Cas. Scaling factors are applied to show the same apparent amplitude; vertical shifts are made for clarity. Approximate measurement errors are indicated. The dashed, tapered line shows the assumed limiting absorption relation (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.9cm,clip]{6639fig2.eps} \end{figure}$ Figure 2: Maximum (upper) and minimum absorption lines of the C IV doublet of $\zeta$ Cas fit with synthetic spectra (dashed lines). Fitting parameters are indicated (see Table 1). The shaded area denotes the emission component determined in the models; the dotted line in the lower plot repeats the maximum absorption profile in this same wavelength range for comparison. The blue wing absorption of the C IV lines is due to the (unmodeled) wind contribution. The rms spectra is also shown.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{6639fig3.eps} \end{figure}$ Figure 3: Maximum (upper) and minimum absorption in the N V doublet lines of $\zeta$ Cas fit with synthetic spectra (dashed lines). Fitting parameters are indicated (see also Table 1). Vestigial emission (shaded area) in $\lambda$ 1242 is suggested in our model.
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In the text

$\begin{figure} \par\includegraphics[height=17cm,width=5.5cm,angle=-90]{6639fig4.eps} \end{figure}$ Figure 4: The geometry at the times of maximum ( $\phi = 0.5$ ) and minimum ( $\phi = 0$ ) absorptions of the resonance lines of $\zeta$ Cas in panels a) and b), respectively. The observer is to the right. The angles $i = 18\hbox {$^\circ $ }$ and $\beta = 79\hbox {$^\circ $ }$ are taken from N03. Low-excitation line absorptions are formed in the optically-thin disk interior. Closed at the outer end, the disk is centered around the magnetic equatorial plane and taken to be an oblate spheroid. The outer edge of the disk is heated by impacts from the high velocity wind and includes superions responsible for the resonance line absorptions. Net redshifted emissions are produced in an "auroral cap'' shown as a dotted region over the magnetic poles (at $\sim$ 11 and $\sim$ 5 o'clock positions).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.7cm,clip]{6639fig1.eps} \end{figure}$	Figure 1: Variation of line strength indices for the UV resonance doublets of N V, Si IV, and C IV with phase in the spectrum of $\zeta$ Cas. Scaling factors are applied to show the same apparent amplitude; vertical shifts are made for clarity. Approximate measurement errors are indicated. The dashed, tapered line shows the assumed limiting absorption relation (see text).
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$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{6639fig3.eps} \end{figure}$	Figure 3: Maximum (upper) and minimum absorption in the N V doublet lines of $\zeta$ Cas fit with synthetic spectra (dashed lines). Fitting parameters are indicated (see also Table 1). Vestigial emission (shaded area) in $\lambda$ 1242 is suggested in our model.
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