All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0086f1.ps}\end{figure}$ Figure 1: The temporal development of the C IV resonant doublet. The data from 1986 are not incorporated in the figure since the doublet was saturated. The three absorption features in early IUE spectra discussed in the text are marked in the figure. The spectra have been shifted in relative intensity for plotting purposes and the intensity of the two uppermost spectra in the figure are multiplied by a factor of two.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0086f2.ps}\end{figure}$ Figure 2: The temporal development of the N V resonant doublet. The intensity of the spectrum recorded on 13 Oct. 1978 is multiplied by a factor of 4 and the spectrum from 9 Jan. 1981 is multiplied by 2. The sharp, deep absorption features in the two uppermost spectra are data artefacts.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{0086f3.eps}\end{figure}$ Figure 3: Scheme showing photoexcitation by an accidental resonance, i.e. $\lambda _{\rm pump} \sim \lambda _{12}$ . A strong line from spectrum X pumps the 1 $\rightarrow$ 2 transition in Y, which results in the fluorescence line 2 $\rightarrow$ 3 with intensity $I_{\rm fl}$ . B₁₂ and A₂₃ are Einstein coefficients.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{0086f4.ps}\end{figure}$ Figure 4: C IV pumped Fe II fluorescence lines $\lambda$ $\lambda$ 2479.98, 2481.80, 2483.08, 2493.10, in AG Peg identified in the IUE spectrum LWP25995 (recorded 25 July 1993).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f5.eps}\end{figure}$ Figure 5: Temporal behaviour of C IV $\lambda$ 1550.78 and the C IV pumped fluorescence of Fe II. The filled circles correspond to the intensity of the Fe II $\lambda$ 2493.10 line pumped by the red giant emission and the triangles correspond to the sum of the intensity of the observed Fe II lines produced by pumping of the white dwarf.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f6.eps}\end{figure}$ Figure 6: Correlation between Fe II fluorescence lines and C IV $\lambda$ 1550.78. Intensites are given in units of 10^-13 erg cm^-2 s^-1 Å^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{0086f7a.ps}\vspace*{5mm} \includegraphics[angle=90,width=8.8cm,clip]{0086f7b.ps}\end{figure}$ Figure 7: The observed spectrum of AG Peg (solid) is compared to the fitted theoretical spectrum (dotted) for the resonance region of C IV (Fig. 7a) and N V (Fig. 7b). The observed spectra were recorded on 9 October 1979 (C IV) and 18 August 1978 (N V).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f8.eps}\end{figure}$ Figure 8: Temporal behaviour of the white dwarf wind velocities of C IV and N V.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f9.eps}\end{figure}$ Figure 9: C IV and N V peak intensities in the white dwarf wind. The last three circles (1994-1995) are to be treated as upper limits. Since the FWHM of the wind profiles was almost constant through the period ( $\sim$ 2.5 Å for N V and $\sim$ 2.1 Å for C IV) the total line fluxes follow the trends of the peak intensities. The sharp absorption at 1242.05 Å is a data artefact.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f10.eps}\end{figure}$ Figure 10: C IV and N V line opacities in the white-dwarf wind in AG Peg.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f11.eps}\end{figure}$ Figure 11: Intensities in the wind-collision region in AG Peg.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f12.eps}\end{figure}$ Figure 12: Opacities in the wind-collision region in AG Peg.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f13.eps}\end{figure}$ Figure 13: Emission intensities from ionized part of red-giant wind in AG Peg.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f14.eps}\end{figure}$ Figure 14: Line opacities in ionized part of red-giant wind in AG Peg.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.2cm,clip]{0086f15a.ps}\vspa... ...pace*{2mm} \includegraphics[angle=90,width=7.2cm,clip]{0086f15d.ps}\end{figure}$ Figure 15: Comparison between observed spectra of AG Peg (solid) and fits (dotted) of the C IV and N V doublets where the Fe II pumping channels (vertical lines) are not included a) or included b).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0086f2.ps}\end{figure}$	Figure 2: The temporal development of the N V resonant doublet. The intensity of the spectrum recorded on 13 Oct. 1978 is multiplied by a factor of 4 and the spectrum from 9 Jan. 1981 is multiplied by 2. The sharp, deep absorption features in the two uppermost spectra are data artefacts.
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$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{0086f3.eps}\end{figure}$	Figure 3: Scheme showing photoexcitation by an accidental resonance, i.e. $\lambda _{\rm pump} \sim \lambda _{12}$ . A strong line from spectrum X pumps the 1 $\rightarrow$ 2 transition in Y, which results in the fluorescence line 2 $\rightarrow$ 3 with intensity $I_{\rm fl}$ . B₁₂ and A₂₃ are Einstein coefficients.
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$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{0086f4.ps}\end{figure}$	Figure 4: C IV pumped Fe II fluorescence lines $\lambda$ $\lambda$ 2479.98, 2481.80, 2483.08, 2493.10, in AG Peg identified in the IUE spectrum LWP25995 (recorded 25 July 1993).
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f5.eps}\end{figure}$	Figure 5: Temporal behaviour of C IV $\lambda$ 1550.78 and the C IV pumped fluorescence of Fe II. The filled circles correspond to the intensity of the Fe II $\lambda$ 2493.10 line pumped by the red giant emission and the triangles correspond to the sum of the intensity of the observed Fe II lines produced by pumping of the white dwarf.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f6.eps}\end{figure}$	Figure 6: Correlation between Fe II fluorescence lines and C IV $\lambda$ 1550.78. Intensites are given in units of 10^-13 erg cm^-2 s^-1 Å^-1.
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$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{0086f7a.ps}\vspace*{5mm} \includegraphics[angle=90,width=8.8cm,clip]{0086f7b.ps}\end{figure}$	Figure 7: The observed spectrum of AG Peg (solid) is compared to the fitted theoretical spectrum (dotted) for the resonance region of C IV (Fig. 7a) and N V (Fig. 7b). The observed spectra were recorded on 9 October 1979 (C IV) and 18 August 1978 (N V).
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f8.eps}\end{figure}$	Figure 8: Temporal behaviour of the white dwarf wind velocities of C IV and N V.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f9.eps}\end{figure}$	Figure 9: C IV and N V peak intensities in the white dwarf wind. The last three circles (1994-1995) are to be treated as upper limits. Since the FWHM of the wind profiles was almost constant through the period ( $\sim$ 2.5 Å for N V and $\sim$ 2.1 Å for C IV) the total line fluxes follow the trends of the peak intensities. The sharp absorption at 1242.05 Å is a data artefact.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f10.eps}\end{figure}$	Figure 10: C IV and N V line opacities in the white-dwarf wind in AG Peg.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f11.eps}\end{figure}$	Figure 11: Intensities in the wind-collision region in AG Peg.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f12.eps}\end{figure}$	Figure 12: Opacities in the wind-collision region in AG Peg.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f13.eps}\end{figure}$	Figure 13: Emission intensities from ionized part of red-giant wind in AG Peg.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0086f14.eps}\end{figure}$	Figure 14: Line opacities in ionized part of red-giant wind in AG Peg.
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$\begin{figure} \par\includegraphics[angle=90,width=7.2cm,clip]{0086f15a.ps}\vspa... ...pace*{2mm} \includegraphics[angle=90,width=7.2cm,clip]{0086f15d.ps}\end{figure}$	Figure 15: Comparison between observed spectra of AG Peg (solid) and fits (dotted) of the C IV and N V doublets where the Fe II pumping channels (vertical lines) are not included a) or included b).
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