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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1996fig1.ps} \end{figure}$ Figure 1: Observed (Adelman 1981) and computed flux distributions. The filled circles represent the energy distribution dereddened with E(B-V)=0.014, the open circles represent the energy distribution dereddened with E(B-V)=0.048. The respective best fit theoretical calculations were obtained for the 8400g35 (full line) and 8700g34 (dashed line) model atmospheres.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1996fg2a.ps}\hspace*{3mm} \includegraphics[width=8cm,clip]{1996fg2b.ps} \end{figure}$ Figure 2: A comparison between the observed (thin line) and computed (full line - the 8400g35 model atmosphere, dashed line - the 8700g34 model atmosphere) H $\gamma$ ( left panel) and H $\beta$ ( right panel) line profiles.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{1996fig3.ps} \end{figure}$ Figure 3: Position of HD 204411 in the HR diagram.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1996fig4.ps} \end{figure}$ Figure 4: The observed (circles) and computed line profiles. For the magnetically insensitive Fe I $\lambda$ 5434.52 line ( top panel) and Fe I $\lambda$ 5576.09 line ( middle panel), the rotationally broadened line profiles ( $v_{\rm e}\sin i$ = 6.3 km s^-1- dashed line) and the profiles (solid line) computed assuming $v_{\rm e}\sin i$ = 5.4 km s^-1and $v_{\rm {macro}}=4.8$ km s^-1 are shown. The bottom panel shows that the observed profile of Fe I $\lambda$ 6149.258 line ( $g_{\rm eff}$ = 1.35) is still slightly more broadened than the profile computed with the previous values of the rotational and macroturbulent velocities (dotted line). It is possible to improve the fit by adding a 750 gauss magnetic field (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1996fig5.ps} \end{figure}$ Figure 5: A comparison between the ELODIE spectrum (circles) and the SARG spectrum (line) convolved with the ${\it FWHM}=0.11$ Å Gaussian profile.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1996fg6a.ps}\hspace*{3mm} \includegraphics[width=8.5cm,clip]{1996fg6b.ps} \end{figure}$ Figure 6: Dependence of the individual abundances on the excitation potential for Fe II lines ( left panel) in HD 204411 (filled circles) and Sirius (asterisks). Dependence of the individual abundances on the equivalent width for Fe II lines with E_i > 10 eV in HD 204411 ( right panel).
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{1996fig7.ps} \end{figure}$ Figure 7: Abundance stratification in the atmosphere of HD 204411.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1996fg8a.ps}\hspace*{3mm} \includegraphics[width=7cm,clip]{1996fg8b.ps} \end{figure}$ Figure 8: A comparison between the observed line profiles and calculations with the stratified abundance distribution (full line) and with the homogeneous abundances (dashed line) from Table 3. The Mg lines ( left panel) and the Si lines ( right panel) are shown in this plot.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1996fig9.ps} \end{figure}$ Figure 9: The same as in Fig. 8 but for Ca.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1996fg10.ps} \end{figure}$ Figure 10: The same as in Fig. 8 but for Cr.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1996fg11.ps} \end{figure}$ Figure 11: The same as in Fig. 8 but for Fe.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1996fig1.ps} \end{figure}$	Figure 1: Observed (Adelman 1981) and computed flux distributions. The filled circles represent the energy distribution dereddened with E(B-V)=0.014, the open circles represent the energy distribution dereddened with E(B-V)=0.048. The respective best fit theoretical calculations were obtained for the 8400g35 (full line) and 8700g34 (dashed line) model atmospheres.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1996fg2a.ps}\hspace*{3mm} \includegraphics[width=8cm,clip]{1996fg2b.ps} \end{figure}$	Figure 2: A comparison between the observed (thin line) and computed (full line - the 8400g35 model atmosphere, dashed line - the 8700g34 model atmosphere) H $\gamma$ ( left panel) and H $\beta$ ( right panel) line profiles.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{1996fig3.ps} \end{figure}$	Figure 3: Position of HD 204411 in the HR diagram.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1996fig5.ps} \end{figure}$	Figure 5: A comparison between the ELODIE spectrum (circles) and the SARG spectrum (line) convolved with the ${\it FWHM}=0.11$ Å Gaussian profile.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1996fg6a.ps}\hspace*{3mm} \includegraphics[width=8.5cm,clip]{1996fg6b.ps} \end{figure}$	Figure 6: Dependence of the individual abundances on the excitation potential for Fe II lines ( left panel) in HD 204411 (filled circles) and Sirius (asterisks). Dependence of the individual abundances on the equivalent width for Fe II lines with E_i > 10 eV in HD 204411 ( right panel).
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{1996fig7.ps} \end{figure}$	Figure 7: Abundance stratification in the atmosphere of HD 204411.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1996fg8a.ps}\hspace*{3mm} \includegraphics[width=7cm,clip]{1996fg8b.ps} \end{figure}$	Figure 8: A comparison between the observed line profiles and calculations with the stratified abundance distribution (full line) and with the homogeneous abundances (dashed line) from Table 3. The Mg lines ( left panel) and the Si lines ( right panel) are shown in this plot.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{1996fig9.ps} \end{figure}$	Figure 9: The same as in Fig. 8 but for Ca.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{1996fg10.ps} \end{figure}$	Figure 10: The same as in Fig. 8 but for Cr.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{1996fg11.ps} \end{figure}$	Figure 11: The same as in Fig. 8 but for Fe.
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