All Figures

$\begin{figure} \par\includegraphics[angle=90,width=15.9cm,clip]{1527fg01.ps} \end{figure}$ Figure 1: The blue light curve before ( top) and after ( bottom) prewhitening the frequencies f₁,f₂,f₃. The four different datasets are indicated.
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In the text

$\begin{figure} \par\includegraphics[height=8.6cm,width=6.8cm,angle=90,clip]{1527fg02.ps} \end{figure}$ Figure 2: Prewhitened y and u-b light- and colour curves (see text). The binary model from Sect. 5 is superimposed.
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In the text

$\begin{figure} \par\includegraphics[height=11.3cm,width=8.1cm,angle=90,clip]{1527fg03.ps} \end{figure}$ Figure 3: The model orbit from RV differences (full line), compared with RVs from cross-correlations with a template (thick lines). For $\gamma =0$ .
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In the text

$\begin{figure} \par\includegraphics[height=6.7cm,width=7cm,clip]{1527fg04.ps} \end{figure}$ Figure 4: Selection of matching pairs (fat dots) among all combinations for the criteria (see text): linear cutoff (line), pair elements separated >4.5 h in time, $I_{\rm SN}>0.90$ and $I_{\rm MM}<0.00139$ . Points along zero ordinate are auto-correlations and pairs with ECHELEC elements.
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In the text

$\begin{figure} \par\includegraphics[height=6.4cm,width=4.1cm,clip]{1527fg05.ps}\... ...{2mm} \includegraphics[width=4.1cm,height=6.4cm,clip]{1527fg06.ps} \end{figure}$ Figure 5: Two-dimensional power spectra for wavelength regions centered on the Si III 4553 Å ( left) and O II 4596 Å ( right) lines. Owing to insufficient data sampling, strong aliasing makes the significant frequencies appear "smeared''. The three photometric frequencies are indicated ("-''). Note the similarity of the periodicities for the two lines.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{1527fg07.eps} \end{figure}$ Figure 6: Summed power spectrum from the combined O II 4596 Å and Si III 4553 Å regions ( top). The three photometric frequencies are indicated with dotted lines. The two lower panels show the power spectra with respectively one (7.1651 $\;{\rm c}~{\rm d}^{-1}$ ) and two (7.1651 and 6.6640 c/d) frequencies prewhitened. Note that power still is present at 5.6597, 6.6620 and 12.8655 $\;{\rm c}~{\rm d}^{-1}$ , indicating an incomplete solution.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1527fg08.ps} \end{figure}$ Figure 7: Integrated-flux variations, in units of normalised flux per pixel, inside a 5-bin wide core region of Si III 4553 Å. The panels show phase diagrams for each of the detected pulsational periods, each successive one after prewhitening for the previous one above. Sinusoidal fits are superimposed for the individual frequencies. The panels show the monochromatic input light curve phased with $f_3=7.1651~\hbox{$\;{\rm c}~{\rm d}^{-1}$ }$ a), then f₃ is prewhitened and the light curve is phased with f₂ b), and c) is for the light curve with f₃ and f₂ prewhitened and phased with a candidate frequency $f=12.8655~\hbox{$\;{\rm c}~{\rm d}^{-1}$ }$ . Note the reduction of the scatter.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{1527fg09.ps} \end{figure}$ Figure 8: Residuals of the uvby light curves from the DC solution with the geometry free (Table 9). Dotted lines delimit the start and end of both eclipses. From top to bottom: y,b,v,u.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1527fg10.ps} \end{figure}$ Figure 9: The positions of the components of HD 92024 in an evolutionary diagram for $\log L$ versus $\log T_{\rm eff}$ from Claret (1995). Error bars are included from Table 12. Dotted lines are isochrones with $\log age$ indicated while the solid lines are evolutionary tracks for different masses.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=15.9cm,clip]{1527fg01.ps} \end{figure}$	Figure 1: The blue light curve before ( top) and after ( bottom) prewhitening the frequencies f₁,f₂,f₃. The four different datasets are indicated.
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$\begin{figure} \par\includegraphics[height=8.6cm,width=6.8cm,angle=90,clip]{1527fg02.ps} \end{figure}$	Figure 2: Prewhitened y and u-b light- and colour curves (see text). The binary model from Sect. 5 is superimposed.
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$\begin{figure} \par\includegraphics[height=11.3cm,width=8.1cm,angle=90,clip]{1527fg03.ps} \end{figure}$	Figure 3: The model orbit from RV differences (full line), compared with RVs from cross-correlations with a template (thick lines). For $\gamma =0$ .
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$\begin{figure} \par\includegraphics[height=6.7cm,width=7cm,clip]{1527fg04.ps} \end{figure}$	Figure 4: Selection of matching pairs (fat dots) among all combinations for the criteria (see text): linear cutoff (line), pair elements separated >4.5 h in time, $I_{\rm SN}>0.90$ and $I_{\rm MM}<0.00139$ . Points along zero ordinate are auto-correlations and pairs with ECHELEC elements.
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$\begin{figure} \par\includegraphics[height=6.4cm,width=4.1cm,clip]{1527fg05.ps}\... ...{2mm} \includegraphics[width=4.1cm,height=6.4cm,clip]{1527fg06.ps} \end{figure}$	Figure 5: Two-dimensional power spectra for wavelength regions centered on the Si III 4553 Å ( left) and O II 4596 Å ( right) lines. Owing to insufficient data sampling, strong aliasing makes the significant frequencies appear "smeared''. The three photometric frequencies are indicated ("-''). Note the similarity of the periodicities for the two lines.
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$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{1527fg09.ps} \end{figure}$	Figure 8: Residuals of the uvby light curves from the `DC` solution with the geometry free (Table 9). Dotted lines delimit the start and end of both eclipses. From top to bottom: y,b,v,u.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1527fg10.ps} \end{figure}$	Figure 9: The positions of the components of HD 92024 in an evolutionary diagram for $\log L$ versus $\log T_{\rm eff}$ from Claret (1995). Error bars are included from Table 12. Dotted lines are isochrones with $\log age$ indicated while the solid lines are evolutionary tracks for different masses.
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