All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{0345f1.ps}\end{figure}$ Figure 1: The dependence of the critical optical depth $\tau _{\rm ross}$ from the magnetic field strength.
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In the text

$\begin{figure} \par\includegraphics[height=10cm,width=8cm,clip]{0345f2a.ps}\vspa... ...0.5cm} \par\includegraphics[height=10cm,width=8cm, clip]{0345f2b.ps}\end{figure}$ Figure 2: The effective gravity versus the Rosseland optical depth for a) the outward- and b) inward-directed Lorentz force.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm, height=8.5cm,clip]{0345f3a.ps}\... ...5cm} \par\includegraphics[width=7.5cm, height=8.5cm]{0345f3b_ac.eps}\end{figure}$ Figure 3: The electron and ion electrical conductivity (logarithmic scale) as a function of the Rosseland optical depth for models No. 5 ( $B_{\rm eq} = 50$ G) and 10 ( $B_{\rm eq} = 500$ G) (dashed curves). The electrical conductivity of the electrons and ions in the absence of magnetic field is shown by solid lines. a) The outward-directed Lorentz force, b) the inward-directed magnetic force.
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In the text

$\begin{figure} \par\includegraphics[width=7cm, height=6cm,clip]{0345f4a.ps}\vspace*{0.5cm} \par\includegraphics[width=7cm, height=6cm,clip]{0345f4b.ps}\end{figure}$ Figure 4: The temperature perturbations in the magnetic models relative to the reference non-magnetic model. a) The outward-directed Lorentz force; b) the inward-directed magnetic force.
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In the text

$\begin{figure} \par\includegraphics[width=7cm, height=9.2cm,clip]{0345f5a.ps}\vs... ....5cm} \par\includegraphics[width=7cm, height=9.2cm,clip]{0345f5b.ps}\end{figure}$ Figure 5: The differences between the magnetic and non-magnetic H $\beta$ profiles. a) The outward-directed Lorentz force; b) the inward-directed magnetic force.
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In the text

$\begin{figure} \par\includegraphics[width=7cm, height=7cm,clip]{0345f6.ps}\end{figure}$ Figure 6: The maximum difference between H $\beta$ profiles computed for magnetic and non-magnetic atmospheres as a function of the magnetic field strength $B_{\rm loc}$ . The solid line illustrates the outward-directed Lorentz force, while the dashed line corresponds to the inward-directed magnetic force.
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In the text

$\begin{figure} \par\includegraphics[width=7cm, height=7cm,clip]{0345f7.ps}\end{figure}$ Figure 7: The maximum difference between H $\beta$ profiles computed for magnetic ( $B_{\rm loc}=500$ G) and non-magnetic atmospheres as a function of the stellar effective temperature. The solid line illustrates the outward-directed Lorentz force, while the dashed line corresponds to the inward-directed magnetic force.
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In the text

$\begin{figure} \par\includegraphics[width=8cm, height=7cm,clip]{0345f8.ps}\end{figure}$ Figure 8: Phase variation of the disk-integrated magnetic parameters for the dipolar field geometry with the polar strength $B_{\rm p} = 1$ kG, $\beta =90\hbox {$^\circ $ }$ and $i=90\hbox {$^\circ $ }$ . The solid line shows the phase curve of the longitudinal field $\langle B_{\rm z}\rangle$ , dashed line corresponds to the field modulus $\langle B\rangle$ and dotted line - to $\langle\sin \theta B_\theta\rangle$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm, height=12.7cm,clip]{0345f9.ps}\end{figure}$ Figure 9: Phase variation of the disk-integrated H $\beta$ profiles for a rotating magnetic star with 1 kG dipolar field and $E_{\rm eq} = 5 \times 10^{-11}$ . Hydrogen line profiles are plotted for phases 0.00, 0.05, 0.10, 0.15 and 0.20 relative to the profile corresponding to the rotational phase 0.25 (strongest magnetic field effect). The upper plot is for the outward-directed Lorentz force, while the lower plot illustrates results for the inward-directed magnetic force.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{0345f10.ps}\end{figure}$ Figure 10: Phase variation of the equivalent width of hydrogen Balmer lines for different stellar inclinations i and magnetic obliquities $\beta$ of the 1 kG dipolar field and $E_{\rm eq} = 5 \times 10^{-11}$ . The thick curves correspond to the outward-directed Lorentz force, while the thin lines show calculations for the inward-directed magnetic force. Dashed lines show variation of H $\alpha$ , solid lines - H $\beta$ and dotted lines - H $\gamma$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0345f1.ps}\end{figure}$	Figure 1: The dependence of the critical optical depth $\tau _{\rm ross}$ from the magnetic field strength.
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$\begin{figure} \par\includegraphics[height=10cm,width=8cm,clip]{0345f2a.ps}\vspa... ...0.5cm} \par\includegraphics[height=10cm,width=8cm, clip]{0345f2b.ps}\end{figure}$	Figure 2: The effective gravity versus the Rosseland optical depth for a) the outward- and b) inward-directed Lorentz force.
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$\begin{figure} \par\includegraphics[width=7cm, height=6cm,clip]{0345f4a.ps}\vspace*{0.5cm} \par\includegraphics[width=7cm, height=6cm,clip]{0345f4b.ps}\end{figure}$	Figure 4: The temperature perturbations in the magnetic models relative to the reference non-magnetic model. a) The outward-directed Lorentz force; b) the inward-directed magnetic force.
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$\begin{figure} \par\includegraphics[width=7cm, height=9.2cm,clip]{0345f5a.ps}\vs... ....5cm} \par\includegraphics[width=7cm, height=9.2cm,clip]{0345f5b.ps}\end{figure}$	Figure 5: The differences between the magnetic and non-magnetic H $\beta$ profiles. a) The outward-directed Lorentz force; b) the inward-directed magnetic force.
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$\begin{figure} \par\includegraphics[width=7cm, height=7cm,clip]{0345f6.ps}\end{figure}$	Figure 6: The maximum difference between H $\beta$ profiles computed for magnetic and non-magnetic atmospheres as a function of the magnetic field strength $B_{\rm loc}$ . The solid line illustrates the outward-directed Lorentz force, while the dashed line corresponds to the inward-directed magnetic force.
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$\begin{figure} \par\includegraphics[width=7cm, height=7cm,clip]{0345f7.ps}\end{figure}$	Figure 7: The maximum difference between H $\beta$ profiles computed for magnetic ( $B_{\rm loc}=500$ G) and non-magnetic atmospheres as a function of the stellar effective temperature. The solid line illustrates the outward-directed Lorentz force, while the dashed line corresponds to the inward-directed magnetic force.
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