All Figures

$\begin{figure} \par\includegraphics[height=4.6cm,width=6.1cm,clip]{7700f01a.eps}... ...*{3mm} \includegraphics[height=4.6cm,width=6.1cm,clip]{7700f01b.eps}\end{figure}$ Figure 1: Intrinsic line profiles calculated with LLmodels and SynthV for $T_{\rm eff}$ = 14 500 K, $\log{g}$ = 4.2, $\epsilon ({\rm Si})$ = -3.0, $\epsilon ({\rm Fe})$ = -3.5. Top: the Si II 6371 Å line. Bottom: the 5316 Å feature consisting of three (5316.225, 5316.615, and 5316.784 Å) Fe II lines.
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In the text

$\begin{figure} \par\includegraphics[height=8.4cm,width=4.7cm,angle=-90,clip]{7700f02.eps}\end{figure}$ Figure 2: Surface map (Mercator projection) of the Si II 6347 Å line strengths in terms of relative EWs derived with MAXENT. The relative EW scale (see text) spans -0.15 (white) to +0.30 (black).
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In the text

$\begin{figure} \par\includegraphics[height=8.3cm,width=4cm,angle=90,clip]{7700f0... ...ncludegraphics[height=8.5cm,width=4.5cm,angle=90,clip]{7700f04f.eps}\end{figure}$ Figure 3: Stellar surface abundance maps in Mercator projection obtained with INVERS8 from the single atmosphere model with different regularization parameters and $T_{\rm eff}$ = 14 500 K, $\log{g}$ = 4.2, $\epsilon ({\rm Si})$ = -3.5, $\epsilon ({\rm Fe})$ = -4.0, $\epsilon ({\rm He})$ = -3.0, $v\sin{i}$ = 100 km s^-1, i = 65 $^{\circ }$ . From top to bottom: $\Lambda$ = 0.01, 0.001, 0.0001. All Si abundances ( left) and all Fe abundances ( right) are shown on a common dynamical scale reaching from -3.55 (white) to -2.42 (black) for Si and from -4.36 (white) to -3.04 (black) for Fe.
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In the text

$\begin{figure} \includegraphics[angle=90,width=8.3cm,clip]{7700f05a.eps}\hspace*{4mm} \includegraphics[angle=90,width=8.3cm,clip]{7700f05b.eps}\end{figure}$ Figure 4: Stellar surface abundance maps in spherical projection for Si II and Fe II using the same atmospheric parameters as in Fig. 3 and $\Lambda$ = 0.0001.
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In the text

$\begin{figure} \par\includegraphics[height=2.5cm,width=9.35cm,angle=90,clip]{770... ...cludegraphics[height=2.5cm,width=9.35cm,angle=90,clip]{7700f03c.eps}\end{figure}$ Figure 5: Comparison between observed (solid) and computed (dash-dotted) line profiles derived with INVERS8 and $\Lambda$ = 0.01. Central line depths in units of the continuum are 0.81, 0.85, and 0.92 for the Si II 6347 and 6371 Å and the Fe II 5316 Å lines, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7700f06.eps}\end{figure}$ Figure 6: Change of the stellar structure due to different abundances. Temperature versus Rosseland opacity calculated for $T_{\rm eff}$ = 14 500 K, $\log{g}$ = 4.2, $\epsilon ({\rm He})= -3.0$ and $\epsilon ({\rm Si})= -3.5$ , $\epsilon ({\rm Fe})= -3.5$ (solid); $\epsilon ({\rm Si})= -2.5$ , $\epsilon ({\rm Fe})= -3.5$ (dotted); and $\epsilon ({\rm Si})= -3.5$ , $\epsilon ({\rm Fe})= -4.0$ (dashed).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.15cm,clip]{7700f07a.eps}\par\includegraphics[angle=90,width=8.15cm,clip]{7700f07b.eps}\end{figure}$ Figure 7: Maps showing the difference of elemental abundances: multiple minus single components atmosphere model.
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In the text

$\begin{figure} \par\includegraphics[width=6.15cm,clip]{7700f08.eps}\end{figure}$ Figure 8: Standard deviation of the H $_\beta$ lines across the H $_\beta$ profile.
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In the text

$\begin{figure} \includegraphics[width=6.35cm,clip]{7700f09a.eps}\vspace*{-2mm} \... ...eps}\vspace*{-2mm} \includegraphics[width=6.35cm,clip]{7700f09d.eps}\end{figure}$ Figure 9: Solid curves: difference between the H $_\beta$ line profiles at phases of maximum and minimum line strength. Dashed curves: difference computed from synthetic spectra for four different sets of model parameters. From top to bottom: models I, II, III, and IV (see Table 1).
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In the text

$\begin{figure} \par\includegraphics[height=4.6cm,width=6.1cm,clip]{7700f01a.eps}... ...*{3mm} \includegraphics[height=4.6cm,width=6.1cm,clip]{7700f01b.eps}\end{figure}$	Figure 1: Intrinsic line profiles calculated with LLmodels and SynthV for $T_{\rm eff}$ = 14 500 K, $\log{g}$ = 4.2, $\epsilon ({\rm Si})$ = -3.0, $\epsilon ({\rm Fe})$ = -3.5. Top: the Si II 6371 Å line. Bottom: the 5316 Å feature consisting of three (5316.225, 5316.615, and 5316.784 Å) Fe II lines.
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$\begin{figure} \par\includegraphics[height=8.4cm,width=4.7cm,angle=-90,clip]{7700f02.eps}\end{figure}$	Figure 2: Surface map (Mercator projection) of the Si II 6347 Å line strengths in terms of relative EWs derived with MAXENT. The relative EW scale (see text) spans -0.15 (white) to +0.30 (black).
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$\begin{figure} \includegraphics[angle=90,width=8.3cm,clip]{7700f05a.eps}\hspace*{4mm} \includegraphics[angle=90,width=8.3cm,clip]{7700f05b.eps}\end{figure}$	Figure 4: Stellar surface abundance maps in spherical projection for Si II and Fe II using the same atmospheric parameters as in Fig. 3 and $\Lambda$ = 0.0001.
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$\begin{figure} \par\includegraphics[height=2.5cm,width=9.35cm,angle=90,clip]{770... ...cludegraphics[height=2.5cm,width=9.35cm,angle=90,clip]{7700f03c.eps}\end{figure}$	Figure 5: Comparison between observed (solid) and computed (dash-dotted) line profiles derived with INVERS8 and $\Lambda$ = 0.01. Central line depths in units of the continuum are 0.81, 0.85, and 0.92 for the Si II 6347 and 6371 Å and the Fe II 5316 Å lines, respectively.
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$\begin{figure} \par\includegraphics[angle=90,width=8.15cm,clip]{7700f07a.eps}\par\includegraphics[angle=90,width=8.15cm,clip]{7700f07b.eps}\end{figure}$	Figure 7: Maps showing the difference of elemental abundances: multiple minus single components atmosphere model.
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$\begin{figure} \par\includegraphics[width=6.15cm,clip]{7700f08.eps}\end{figure}$	Figure 8: Standard deviation of the H $_\beta$ lines across the H $_\beta$ profile.
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$\begin{figure} \includegraphics[width=6.35cm,clip]{7700f09a.eps}\vspace{-2mm} \... ...eps}\vspace{-2mm} \includegraphics[width=6.35cm,clip]{7700f09d.eps}\end{figure}$	Figure 9: Solid curves: difference between the H $_\beta$ line profiles at phases of maximum and minimum line strength. Dashed curves: difference computed from synthetic spectra for four different sets of model parameters. From top to bottom: models I, II, III, and IV (see Table 1).
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