All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0253f1.eps} \end{figure}$ Figure 1: The radial-velocity curve of $\kappa~$ Sco for 1-d RV normals. The RVs from older photographic spectra are shown by empty circles.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0253f2a.eps}\par\vspace*{4mm} \includegraphics[width=8.7cm,clip]{0253f2b.eps} \end{figure}$ Figure 2: The radial-velocity curve of $\kappa~$ Sco for all 699 individual spectra (circles) based on KOREL disentangling. The upper panel shows the RV curves of both binary components (secondary by empty symbols) while the bottom panel shows the same RV curve for the primary only for clarity. The data are plotted with respect to ephemeris from the KOREL solution $T_{\rm periastr.}$ = HJD 2 449 984.18 + 195 $^{\hbox{$.\!\!^{\rm d}$ }}$ 4579 $\times$ E.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0253f3a.eps}\par\vspace*{2mm} \includegraphics[width=8.5cm,clip]{0253f3b.eps} \end{figure}$ Figure 3: The spectrum obtained at one elongation on HJD 2 450 742.4691 is first compared with the disentangled Si III line profile of the primary shifted in RV for +52.8 km s^-1 ( upper panel). The residual spectrum after subtraction of the disentangled profile of the primary is compared with the disentangled profile of the secondary shifted for -58.5 km s^-1 ( bottom panel).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0253f4a.eps}\par\vspace*{2mm} \includegraphics[width=8.5cm,clip]{0253f4b.eps} \end{figure}$ Figure 4: The spectrum obtained at the other elongation on HJD 2 450 194.9224 is first compared with the disentangled Si III line profile of the primary shifted in RV for -56.1 km s^-1 ( upper panel). The residual spectrum after subtraction of the disentangled profile of the primary is compared with the disentangled profile of the secondary shifted for +62.0 km s^-1 ( bottom panel).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0253f5.eps} \end{figure}$ Figure 5: Residual line profiles from the spectra taken during the night of 20 July 1997 (HJD 2 450 650) after KOREL disentangling. The left ( right) panel shows the profiles in the rest frame of the primary (secondary). The disentangled Si III profile of the primary (secondary) is shown at the bottom of the panel. Time runs from the bottom to the top.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0253f6.eps} \end{figure}$ Figure 6: The maximum and minimum radius of the primary estimated from the Hipparcos parallax are compared with Schaller's et al. (1992) evolutionary models. Masses of the models for the zero-age and terminal-age main sequence are given.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0253f7.eps} \end{figure}$ Figure 7: Stellingwerf's (1978) $\theta$ statistics for the Hipparcos $H_{\rm p}$ photometry, the RV residuals from the orbit of the primary and for the line intensities of the primary obtained from the KOREL solution, prewhitened for their secular change. One can see the pronounced differences between these periodograms.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0253f8a.eps}\par\vspace*{2mm} \includegraphics[width=8.6cm,clip]{0253f8b.eps} \end{figure}$ Figure 8: The Hipparcos $H_{\rm p}$ photometry, transformed to V magnitude ( upper panel) and line intensity variation of the primary from KOREL expressed in magnitudes ( bottom panel), plotted vs. phase for the ephemeris of the sinusoidal fit to line intensity: $T_{\rm min.light}$ = HJD 2 449 984.1332(41) + 0 $^{\hbox{$.\!\!^{\rm d}$ }}$ 1998277(15) $\times$ E.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0253f9.eps} \end{figure}$ Figure 9: The RV $\rm O{-}C$ residuals from the KOREL solution plotted vs. phase for the ephemeris of the sinusoidal fit to them: $T_{{\rm max} RV}$ = HJD 2 449 984.0982(23) +0 $^{\hbox{$.\!\!^{\rm d}$ }}$ 20003022(84) $\times$ E.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0253f1.eps} \end{figure}$	Figure 1: The radial-velocity curve of $\kappa~$ Sco for 1-d RV normals. The RVs from older photographic spectra are shown by empty circles.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0253f3a.eps}\par\vspace*{2mm} \includegraphics[width=8.5cm,clip]{0253f3b.eps} \end{figure}$	Figure 3: The spectrum obtained at one elongation on HJD 2 450 742.4691 is first compared with the disentangled Si III line profile of the primary shifted in RV for +52.8 km s^-1 ( upper panel). The residual spectrum after subtraction of the disentangled profile of the primary is compared with the disentangled profile of the secondary shifted for -58.5 km s^-1 ( bottom panel).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0253f4a.eps}\par\vspace*{2mm} \includegraphics[width=8.5cm,clip]{0253f4b.eps} \end{figure}$	Figure 4: The spectrum obtained at the other elongation on HJD 2 450 194.9224 is first compared with the disentangled Si III line profile of the primary shifted in RV for -56.1 km s^-1 ( upper panel). The residual spectrum after subtraction of the disentangled profile of the primary is compared with the disentangled profile of the secondary shifted for +62.0 km s^-1 ( bottom panel).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0253f5.eps} \end{figure}$	Figure 5: Residual line profiles from the spectra taken during the night of 20 July 1997 (HJD 2 450 650) after KOREL disentangling. The left ( right) panel shows the profiles in the rest frame of the primary (secondary). The disentangled Si III profile of the primary (secondary) is shown at the bottom of the panel. Time runs from the bottom to the top.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0253f6.eps} \end{figure}$	Figure 6: The maximum and minimum radius of the primary estimated from the Hipparcos parallax are compared with Schaller's et al. (1992) evolutionary models. Masses of the models for the zero-age and terminal-age main sequence are given.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0253f7.eps} \end{figure}$	Figure 7: Stellingwerf's (1978) $\theta$ statistics for the Hipparcos $H_{\rm p}$ photometry, the RV residuals from the orbit of the primary and for the line intensities of the primary obtained from the KOREL solution, prewhitened for their secular change. One can see the pronounced differences between these periodograms.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0253f8a.eps}\par\vspace*{2mm} \includegraphics[width=8.6cm,clip]{0253f8b.eps} \end{figure}$	Figure 8: The Hipparcos $H_{\rm p}$ photometry, transformed to V magnitude ( upper panel) and line intensity variation of the primary from KOREL expressed in magnitudes ( bottom panel), plotted vs. phase for the ephemeris of the sinusoidal fit to line intensity: $T_{\rm min.light}$ = HJD 2 449 984.1332(41) + 0 $^{\hbox{$.\!\!^{\rm d}$ }}$ 1998277(15) $\times$ E.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0253f9.eps} \end{figure}$	Figure 9: The RV $\rm O{-}C$ residuals from the KOREL solution plotted vs. phase for the ephemeris of the sinusoidal fit to them: $T_{{\rm max} RV}$ = HJD 2 449 984.0982(23) +0 $^{\hbox{$.\!\!^{\rm d}$ }}$ 20003022(84) $\times$ E.
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