All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5274F01.eps}\end{figure}$ Figure 1: Upper panel: RV curves of both binary components for solution 4. Bottom panel: the RV curve of the blue-shifted H ${\alpha }$ absorption core. The RVs of the primary and secondary are shown by filled and empty circles, respectively, and those of the H ${\alpha }$ absorption by diamonds.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5274F02.eps}\end{figure}$ Figure 2: DAO RVs (filled circles) and Ondrejov RVs (empty circles) of star 1 plotted vs. time. Small systematic deviations from a smooth orbital RV curve are seen and data from two independent spectrographs prove their reality.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{5274F03.eps}\end{figure}$ Figure 3: Selected H ${\alpha }$ line profiles from the DAO spectrograms showing the presence of a blue-shifted absorption of variable strength throughout the whole orbital cycle. Note that at phases when the line gets very weak, it is also blended with a telluric line at 6557 $\AA$ . The plot is constructed so as to permit a direct comparison with Fig. 8 of Frame et al. (1995). Note that the DAO spectra have a better spectral resolution than the Ondrejov spectra. For comparison, we also show 1 Ondrejov spectrogram taken at HJD 2 453 637.241. One can see that it nicely matches a DAO spectrogram taken shortly thereafter at HJD 2 453 637.659, which indicates that the line intensities from both data sets can be combined safely. (Note that a mean HJD is given for these two spectra in the plot.)
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5274F04A.eps}\vspace*{3mm} \includegraphics[width=8.3cm,clip]{5274F04B.eps}\end{figure}$ Figure 4: Central intensities of the blue-shifted H ${\alpha }$ absorption vs. phase of ephemeris (1): upper panel: our new DAO (filled circles) and Ondrejov (empty circles) electronic spectra; bottom panel: our measurements in the published H ${\alpha }$ line profiles from Hack (1960), Nariai (1967), and Frame et al. (1995). One can see that the line indeed attains a maximum strength (i.e. minimal $I_{\rm c}$ ) at the conjunction with star 2 in front and a minimum at the other conjunction.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.35cm,clip]{5274F05.eps}\end{figure}$ Figure 5: Blue-shifted absorption lines of several Balmer lines from the Ondrejov CCD spectrograms. The same blue shift is observed for all three Balmer lines from similar orbital phases. Note also a good coherence of the phase variations of H ${\alpha }$ and H $\gamma$ ; HJD, cycle numbers, and phases are indicated as in Fig. 3. A line that looks like a blue satellite to He I 6678 moves in phase with it and represents therefore another spectral line of star 1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.45cm,clip]{5274F06.eps}\end{figure}$ Figure 6: The RV curve of a blue-shifted H $\beta$ absorption from Plaskett (1926). The original values were brought on the absolute velocity scale and shifted by 272 km s^-1 to make the curve directly comparable to that shown in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{5274F07.eps}\end{figure}$ Figure 7: Orbital RV curve of the H ${\alpha }$ emission peak.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5274F08.eps}\end{figure}$ Figure 8: A comparison of two Ondrejov H ${\alpha }$ line profiles taken shortly after one elongation and near the conjuction with star 1 in front.
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In the text

$\begin{figure} \par\includegraphics[width=18.4cm,clip]{5274F09.eps}\end{figure}$ Figure 9: Several orbital light curves for the V-magnitude observations found in the astronomical literature.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5274F10.eps}\end{figure}$ Figure 10: A phase plot of Malcolm & Bell (1986) V photometry for the best "period'' of $40\hbox{$.\!\!^{\rm d}$ }9611$ . Two minima of different width in one cycle are seen.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5274F01.eps}\end{figure}$	Figure 1: Upper panel: RV curves of both binary components for solution 4. Bottom panel: the RV curve of the blue-shifted H ${\alpha }$ absorption core. The RVs of the primary and secondary are shown by filled and empty circles, respectively, and those of the H ${\alpha }$ absorption by diamonds.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5274F02.eps}\end{figure}$	Figure 2: DAO RVs (filled circles) and Ondrejov RVs (empty circles) of star 1 plotted vs. time. Small systematic deviations from a smooth orbital RV curve are seen and data from two independent spectrographs prove their reality.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.45cm,clip]{5274F06.eps}\end{figure}$	Figure 6: The RV curve of a blue-shifted H $\beta$ absorption from Plaskett (1926). The original values were brought on the absolute velocity scale and shifted by 272 km s^-1 to make the curve directly comparable to that shown in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.45cm,clip]{5274F07.eps}\end{figure}$	Figure 7: Orbital RV curve of the H ${\alpha }$ emission peak.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5274F08.eps}\end{figure}$	Figure 8: A comparison of two Ondrejov H ${\alpha }$ line profiles taken shortly after one elongation and near the conjuction with star 1 in front.
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$\begin{figure} \par\includegraphics[width=18.4cm,clip]{5274F09.eps}\end{figure}$	Figure 9: Several orbital light curves for the V-magnitude observations found in the astronomical literature.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5274F10.eps}\end{figure}$	Figure 10: A phase plot of Malcolm & Bell (1986) V photometry for the best "period'' of $40\hbox{$.\!\!^{\rm d}$ }9611$ . Two minima of different width in one cycle are seen.
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