All Figures

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{ms3985.f1} \end{figure}$ Figure 1: Light variation of HD 6226 in the V passband plotted vs. time. Frequent light brightenings are clearly seen. All individual observations are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{ms3985.f2} \end{figure}$ Figure 2: The (U-B) vs. (B-V) diagram with all individual $U\!B{}V$ observations of HD 6226 shown by black dots. Also shown are standard sequences for normal dwarfs and bright supergiants. It is clearly seen that HD 6226 is a reddened star and exhibits colour behaviour typical of a positive correlation between light and emission strength as defined by Harmanec (1983).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3985.f3} \end{figure}$ Figure 3: Light variation of HD 6226 in the V passband plotted vs. phase of the 630 $^{\rm d}\!\!.$ 3 period. One can see that the major light brightenings clearly occur on that time scale but their strength varies from one cycle to another.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3985.f4a}\vspace*{4mm} \includegraphics[width=8.6cm,clip]{ms3985.f4b} \end{figure}$ Figure 4: The 2003 emission-line episode of HD 6226: Upper panel: V magnitude vs. time. Bottom panel: Peak intensity (V+R)/2 of the H $\alpha$ emission vs. time.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3985.f5} \end{figure}$ Figure 5: A plot of the V magnitude vs. time for the period covered by the 1997 spectral observations.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{ms3985.f6} \end{figure}$ Figure 6: A plot of the V magnitude vs. time for the period covered when the emission of HD 6226 was first observed on JD 2 451 860.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{ms3985.f7} \end{figure}$ Figure 7: A representative selection of the 1997 and 2003 H $\alpha$ and C II 6578 & 6582 line profiles of HD 6226.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{ms3985.f8} \end{figure}$ Figure 8: A representative selection of the 1997 and 2003 He I 6678 line profiles of HD 6226. Note the pronounced and variable line asymmetry.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3985.f9a}\vspace*{2mm} \... ...85.f9d}\vspace*{2mm} \includegraphics[width=8.8cm,clip]{ms3985.f9e} \end{figure}$ Figure 9: Radial-velocity variations of different measured features plotted vs. phase of the 2 $^{\rm d}\!\!.$ 61507 period for ephemeris (2).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3985.f10} \end{figure}$ Figure 10: The Ondrejov He I 6678 line profile obtained on HJD 2 452 861.3761 (solid line) and a difference between this profile and a profile obtained 0 $^{\rm d}\!\!.$ 233 later (dotted line). A typical signature of moving sub-features is seen.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3985.11a}\vspace*{3mm} \... ...85.11d}\vspace*{3mm} \includegraphics[width=8.8cm,clip]{ms3985.11e} \end{figure}$ Figure 11: A comparison of the 1997 Heros spectrogram of HD 6226 with a synthetic spectrum for 17000 K and $\log~g=3.0$ [cgs] broadened to v sin i = 70 km s^-1. Al wavelengths are in Å. Apart from the He I 6678 line, prone to NLTE effects, the agreement is generally very satisfactory.
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{ms3985.f1} \end{figure}$	Figure 1: Light variation of HD 6226 in the V passband plotted vs. time. Frequent light brightenings are clearly seen. All individual observations are shown.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{ms3985.f2} \end{figure}$	Figure 2: The (U-B) vs. (B-V) diagram with all individual $U\!B{}V$ observations of HD 6226 shown by black dots. Also shown are standard sequences for normal dwarfs and bright supergiants. It is clearly seen that HD 6226 is a reddened star and exhibits colour behaviour typical of a positive correlation between light and emission strength as defined by Harmanec (1983).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3985.f3} \end{figure}$	Figure 3: Light variation of HD 6226 in the V passband plotted vs. phase of the 630 $^{\rm d}\!\!.$ 3 period. One can see that the major light brightenings clearly occur on that time scale but their strength varies from one cycle to another.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3985.f4a}\vspace*{4mm} \includegraphics[width=8.6cm,clip]{ms3985.f4b} \end{figure}$	Figure 4: The 2003 emission-line episode of HD 6226: Upper panel: V magnitude vs. time. Bottom panel: Peak intensity (V+R)/2 of the H $\alpha$ emission vs. time.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3985.f5} \end{figure}$	Figure 5: A plot of the V magnitude vs. time for the period covered by the 1997 spectral observations.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{ms3985.f6} \end{figure}$	Figure 6: A plot of the V magnitude vs. time for the period covered when the emission of HD 6226 was first observed on JD 2 451 860.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{ms3985.f7} \end{figure}$	Figure 7: A representative selection of the 1997 and 2003 H $\alpha$ and C II 6578 & 6582 line profiles of HD 6226.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{ms3985.f8} \end{figure}$	Figure 8: A representative selection of the 1997 and 2003 He I 6678 line profiles of HD 6226. Note the pronounced and variable line asymmetry.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3985.f9a}\vspace{2mm} \... ...85.f9d}\vspace{2mm} \includegraphics[width=8.8cm,clip]{ms3985.f9e} \end{figure}$	Figure 9: Radial-velocity variations of different measured features plotted vs. phase of the 2 $^{\rm d}\!\!.$ 61507 period for ephemeris (2).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms3985.f10} \end{figure}$	Figure 10: The Ondrejov He I 6678 line profile obtained on HJD 2 452 861.3761 (solid line) and a difference between this profile and a profile obtained 0 $^{\rm d}\!\!.$ 233 later (dotted line). A typical signature of moving sub-features is seen.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3985.11a}\vspace{3mm} \... ...85.11d}\vspace{3mm} \includegraphics[width=8.8cm,clip]{ms3985.11e} \end{figure}$	Figure 11: A comparison of the 1997 Heros spectrogram of HD 6226 with a synthetic spectrum for 17000 K and $\log~g=3.0$ [cgs] broadened to v sin i = 70 km s^-1. Al wavelengths are in Å. Apart from the He I 6678 line, prone to NLTE effects, the agreement is generally very satisfactory.
Open with DEXTER