All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{figures/9134fig1.eps}\end{figure}$ Figure 1: Difference in temperature ( upper panel) and gas pressure ( bottom panel) of the models calculated with individual abundances (solid line) and with individual abundances+magnetic field (dashed line) with respect to the reference model atmosphere computed with scaled-solar abundances ([M/H] =+1). For all models $T_{\rm eff}=12~750$ K and $\log g=3.8$ are adopted.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{figures/9134fig2.eps}\end{figure}$ Figure 2: Observed and calculated H $\beta$ line profiles. Upper panel: thick line - UVES observations (1); thin line - the model with solar-scaled abundances [M/H] =+1; dashed line - the model with individual abundances; dotted line - the model with both individual abundances and the magnetic field. Bottom panel: difference (in per sent) between model with only individual abundances (solid line) and with individual abundance+magnetic field (dotted line) relative to the scaled-solar abundance model ( $T_{\rm eff}=12~750$ K, $\log g=3.8$ for all models).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{figures/9134fig3.eps}\end{figure}$ Figure 3: Same as in Fig. 2 but for the H $\gamma$ line.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{figures/9134fig4.eps}\end{figure}$ Figure 4: Influence of magnetic model structure on the profiles of selected spectral lines for $T_{\rm eff}=12~750$ K, $\log g=4.0$ models. Double line - UVES observations; thin line - spectra calculated using the non-magnetic atmospheric model; dashed line - with the magnetic field included.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{figures/9134fig5.eps}\end{figure}$ Figure 5: Theoretical energy distributions for the models with $T_{\rm eff}=12~750$ K, $\log g=3.8$ . Solid line - scaled-solar abundance model, dotted line - the model with individual chemical composition, dashed line - the model with individual abundances and the magnetic field. Energy distributions are convolved with a Gaussian profile with ${\it FWHM}=15$ Å.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{figures/9134fig6.eps}\end{figure}$ Figure 6: Comparison between the observed and calculated fluxes of HD 137509 in the near UV ( upper panel) and visual region ( lower panel). Gaussian smearing with resolution R=1500is applied to all the spectra to provide a better view. In the upper plot the fluxes for the non-magnetic model are shifted along the vertical axis to match the observed spectrum.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{figures/9134fig1.eps}\end{figure}$	Figure 1: Difference in temperature ( upper panel) and gas pressure ( bottom panel) of the models calculated with individual abundances (solid line) and with individual abundances+magnetic field (dashed line) with respect to the reference model atmosphere computed with scaled-solar abundances ([M/H] =+1). For all models $T_{\rm eff}=12~750$ K and $\log g=3.8$ are adopted.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{figures/9134fig3.eps}\end{figure}$	Figure 3: Same as in Fig. 2 but for the H $\gamma$ line.
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$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{figures/9134fig4.eps}\end{figure}$	Figure 4: Influence of magnetic model structure on the profiles of selected spectral lines for $T_{\rm eff}=12~750$ K, $\log g=4.0$ models. Double line - UVES observations; thin line - spectra calculated using the non-magnetic atmospheric model; dashed line - with the magnetic field included.
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$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{figures/9134fig5.eps}\end{figure}$	Figure 5: Theoretical energy distributions for the models with $T_{\rm eff}=12~750$ K, $\log g=3.8$ . Solid line - scaled-solar abundance model, dotted line - the model with individual chemical composition, dashed line - the model with individual abundances and the magnetic field. Energy distributions are convolved with a Gaussian profile with ${\it FWHM}=15$ Å.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{figures/9134fig6.eps}\end{figure}$	Figure 6: Comparison between the observed and calculated fluxes of HD 137509 in the near UV ( upper panel) and visual region ( lower panel). Gaussian smearing with resolution R=1500is applied to all the spectra to provide a better view. In the upper plot the fluxes for the non-magnetic model are shifted along the vertical axis to match the observed spectrum.
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