All Figures

$\begin{figure} \par\includegraphics[width=10.2cm,clip]{ms2901f1.eps} \end{figure}$ Figure 1: Nightly mean H $\alpha$ , He I, and DNa I profiles observed in HD 31648 on the following dates: a) 1/2.11.96; b) 5/6.11.96; c) 28/29.03.97; d) 31.03/1.04.97; e) 28/29.03.98; f) 30/31.03.98; g) 31.03/1.04.98; h) 3/4.04.98. The radial velocity scale is given with respect to the star. For the sake of comparison, the H $\alpha$ profiles obtained on 1/2.11.96, 28/29.03.97, and 28/29.03.98 are also superimposed as dotted lines on the profiles of the consequent observing nights. The dashed lines in the right panel show the continuum level.
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In the text

$\begin{figure} \par\includegraphics[width=10.2cm,clip]{ms2901f2.eps} \end{figure}$ Figure 2: The same as Fig. 1, but for October 1998. Dates of observations are indicated in the figure. The dotted line shows the H $\alpha$ profile obtained on 20.10.
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In the text

$\begin{figure} \par\includegraphics[width=10.2cm,clip]{ms2901f3.eps} \end{figure}$ Figure 3: The same as Fig. 1, but for dates: a) 23/24.03.99; b) 26/27.03.99; c) 28/29.03.99. The dotted line shows the H $\alpha$ profile obtained on 23.03.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms2901f4.eps}\end{figure}$ Figure 4: Nightly mean H $\beta$ profiles observed in HD 31648 in 1998. Dates of observations are indicated in the figure. The dashed lines show the profiles obtained on 30.03 and 20.10 which are superimposed on the profiles of the respectively next observing nights.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{ms2901f5.eps}\end{figure}$ Figure 5: Rapid variations of the He I, H $\alpha$ , and DNa I line profiles observed in HD 31648 during the night 1/2.11.96. The dashed lines show the first in the series He I line profile superimposed on the other profiles for comparison ( left). The residuals with respect to the nightly mean profile are given for the H $\alpha$ and DNa I lines ( middle and right). The short-dashed and long-dashed lines indicate velocity positions for respectively "standing'' and "moving'' waves on the profiles.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{ms2901f6.eps}\end{figure}$ Figure 6: Top: the Stokes parameters of HD 31648 in different passbands averaged for all observing seasons (filled circles). The open circle represents the end of the grey component vector (with error bars from the least squares method) and the initial point of the selective component vectors. The solid and dashed arrows indicate the vector of the grey component and the direction of the selective component (the same in all the passbands), respectively. The error bars in both panels show $\pm \sigma$ -level. Bottom: the wavelength dependence of the selective component. The line is drawn for the law $P(\lambda )\propto \lambda ^{-1}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{ms2901f7.eps}}\end{figure}$ Figure 7: Variations of the polarization q,u-parameters of HD 31648 detected in the UBVRI-passbands in November 1996. The solid lines show trends of variations driven by means of the median-method.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{ms2901f8.eps}}\end{figure}$ Figure 8: Trends of the polarimetric variability of HD 31648 in the UBVRI - passbands on the q,u-plane which were observed in November, 1996. Arrows indicate the direction of time increasing. The dotted lines mark the error levels ( $\pm \sigma$ ) for each trend, which weredetermined by means of the least-squares method.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{ms2901f9.eps}}\end{figure}$ Figure 9: Schematic geometry of the envelope near a Herbig Ae star in the form of a meridional section through the rotation axis. The equatorial accretion disk and the high-latitude boundary of the wind zone in three positions A, B and C are displayed. The cases A, B and C correspond, respectively, to three types of the line profile, usually observed in HAEBEs: A-P Cyg II; B-P Cyg III; C-a single peak. The arrows indicate directions of gaseous flows in the disk and the wind.
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In the text

$\begin{figure} \par\includegraphics[width=10.2cm,clip]{ms2901f2.eps} \end{figure}$	Figure 2: The same as Fig. 1, but for October 1998. Dates of observations are indicated in the figure. The dotted line shows the H $\alpha$ profile obtained on 20.10.
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$\begin{figure} \par\includegraphics[width=10.2cm,clip]{ms2901f3.eps} \end{figure}$	Figure 3: The same as Fig. 1, but for dates: a) 23/24.03.99; b) 26/27.03.99; c) 28/29.03.99. The dotted line shows the H $\alpha$ profile obtained on 23.03.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms2901f4.eps}\end{figure}$	Figure 4: Nightly mean H $\beta$ profiles observed in HD 31648 in 1998. Dates of observations are indicated in the figure. The dashed lines show the profiles obtained on 30.03 and 20.10 which are superimposed on the profiles of the respectively next observing nights.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{ms2901f7.eps}}\end{figure}$	Figure 7: Variations of the polarization q,u-parameters of HD 31648 detected in the UBVRI-passbands in November 1996. The solid lines show trends of variations driven by means of the median-method.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{ms2901f8.eps}}\end{figure}$	Figure 8: Trends of the polarimetric variability of HD 31648 in the UBVRI - passbands on the q,u-plane which were observed in November, 1996. Arrows indicate the direction of time increasing. The dotted lines mark the error levels ( $\pm \sigma$ ) for each trend, which weredetermined by means of the least-squares method.
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