All Figures

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{7141f1.eps}\end{figure}$ Figure 1: Radial velocities of Nova Scorpii 1994 folded on the orbital solution of the data with best fitting sinusoid. Individual velocity errors are ${\protect\la}$ 1.5 ${\rm km}~{\rm s}^{-1}$ and are not plotted because they are always smaller than the symbol size. The bottom panel shows the residuals of the fit.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f2.eps}\end{figure}$ Figure 2: Observed spectrum of the secondary star of Nova Scorpii 1994 ( top) and of a properly broadened template (HIP 46583, bottom).
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{7141f3.eps}\end{figure}$ Figure 3: Distributions obtained for each parameter using Monte Carlo simulations. The labels at the top of each bin indicate the number of simulations consistent with the bin value. The total number of simulations was 1000.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f4.eps}\end{figure}$ Figure 4: Best synthetic spectral fits to the UVES spectrum of the secondary star in the Nova Scorpii 1994 system ( bottom panel) and the same for a template star (properly broadened) shown for comparison ( top panel). Synthetic spectra are computed for solar abundance ratios ( ${\rm [E/Fe]}=0$ with ${\rm [Fe/H]}=-0.1$ , dashed line) and best fit abundance (solid line).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f5.eps}\end{figure}$ Figure 5: The same as in Fig. 4, but for the spectral range $\lambda \lambda 6275$ -6400 Å.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,height=7.9cm,angle=90,clip]{7141... ...includegraphics[width=5.5cm,height=7.7cm,angle=90,clip]{7141f6b.eps}\end{figure}$ Figure 6: The same as in Fig. 4, but for the spectral range $\lambda \lambda 6141$ -6172 Å ( left panels) and $\lambda \lambda 5521$ -5559 Å ( right panels).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.3cm,clip]{7141f7a.eps}\hspace*{4mm} \includegraphics[angle=90,width=7.3cm,clip]{7141f7b.eps}\end{figure}$ Figure 7: The same as in Fig. 4, but for the spectral range $\lambda \lambda 6099$ -6135 Å ( left panels) and $\lambda \lambda 6426$ -6454 Å ( right panels).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f8.eps}\end{figure}$ Figure 8: The same as in Fig. 4, but for the spectral range $\lambda \lambda 6690$ -6760 Å.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f9.eps}\end{figure}$ Figure 9: Upper panel: observed UVES spectrum of the secondary star in comparison with the average synthetic spectrum computed with L INB ROD (dashed line) for all orbital phases and the synthetic spectrum computed with MOOG (solid line). An abundance of [Mg/H $]\sim 0.3$ dex has been adopted for all synthetic spectra. Bottom panel: synthetic spectra computed with L INB ROD for different orbital phases.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f10.eps}\end{figure}$ Figure 10: Upper panel: observed UVES spectrum of the secondary star in comparison with the average synthetic spectrum computed with L INB ROD (dashed line) for all orbital phases and the synthetic spectrum computed with MOOG (solid line). The same element abundances have been adopted for all synthetic spectra. Bottom panel: synthetic spectra computed with L INB ROD for different orbital phases.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=15.5cm,clip]{7141f11.eps}\end{figure}$ Figure 11: Abundance ratios of the secondary star in Nova Scorpii 1994 (blue wide cross) in comparison with the abundances of G and K metal-rich dwarf stars. Galactic trends were taken from Ecuvillon et al. (2004), Ecuvillon et al. (2006) and Gilli et al. (2006). The size of the cross indicates the 1-sigma uncertainty. Filled and empty circles correspond to abundances for planet host stars and stars without known planet companions, respectively. For the abundance of oxygen in metal-rich dwarfs we have only considered abundance measurements in NLTE for the triplet O I 7771-5 Å. The dashed-dotted lines indicate solar abundance values.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7141f12a.eps}\hspace*{4mm} \includegraphics[width=8cm,clip]{7141f12b.eps}\end{figure}$ Figure 12: Left panel: observed abundances (filled circles with the error bars) in comparison with the expected abundances in the secondary star after having captured the 70% of the matter ejected within the solid angle subtended by the secondary from a spherically symmetric supernova explosion of kinetic energy E_K = 10⁵¹ erg for two different mass-cuts, $M_{\rm cut}=2$ ${M}_\odot$ (solid line with open circles), and $M_{\rm cut}=2.54$ ${M}_\odot$ (dashed-dotted line with open circles). Right panel: the same as left panel but for a spherically symmetric hypernova explosion of kinetic energy $E_K = 20\times 10^{51}$ erg for two different mass-cuts, $M_{\rm cut}=3.04$ ${M}_\odot$ (solid line with open circles), and $M_{\rm cut}=4.05$ ${M}_\odot$ (dashed-dotted line with open circles).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7141f13a.eps}\hspace*{4mm} \includegraphics[width=8cm,clip]{7141f13b.eps}\end{figure}$ Figure 13: Left panel: observed abundances (filled circles with the error bars) in comparison with the expected abundances in the secondary star after having captured the 10% of the matter ejected within the solid angle subtended by the secondary from a non-spherically symmetric supernova explosion of kinetic energy E_K = 10⁵² erg for two different mass-cuts, $M_{\rm cut}=2.41$ ${M}_\odot$ (solid line with open circles), and $M_{\rm cut}=2.66$ ${M}_\odot$ (dashed-dotted line with open circles). This model corresponds to the matter ejected in the equatorial plane of the primary where we assumed that the secondary star is located (see more details in González Hernández et al. 2005b). Right panel: the same as left panel but in this model we have assumed complete lateral mixing where all the material within given velocity bins is assumed to be completely mixed. Two simulations are shown for two different mass-cuts, $M_{\rm cut}=2.41$ ${M}_\odot$ (solid line with open circles), and $M_{\rm cut}=5.14$ ${M}_\odot$ (dashed-dotted line with open circles).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{7141f1.eps}\end{figure}$	Figure 1: Radial velocities of Nova Scorpii 1994 folded on the orbital solution of the data with best fitting sinusoid. Individual velocity errors are ${\protect\la}$ 1.5 ${\rm km}~{\rm s}^{-1}$ and are not plotted because they are always smaller than the symbol size. The bottom panel shows the residuals of the fit.
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$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f2.eps}\end{figure}$	Figure 2: Observed spectrum of the secondary star of Nova Scorpii 1994 ( top) and of a properly broadened template (HIP 46583, bottom).
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$\begin{figure} \par\includegraphics[width=11cm,clip]{7141f3.eps}\end{figure}$	Figure 3: Distributions obtained for each parameter using Monte Carlo simulations. The labels at the top of each bin indicate the number of simulations consistent with the bin value. The total number of simulations was 1000.
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$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f4.eps}\end{figure}$	Figure 4: Best synthetic spectral fits to the UVES spectrum of the secondary star in the Nova Scorpii 1994 system ( bottom panel) and the same for a template star (properly broadened) shown for comparison ( top panel). Synthetic spectra are computed for solar abundance ratios ( ${\rm [E/Fe]}=0$ with ${\rm [Fe/H]}=-0.1$ , dashed line) and best fit abundance (solid line).
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$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f5.eps}\end{figure}$	Figure 5: The same as in Fig. 4, but for the spectral range $\lambda \lambda 6275$ -6400 Å.
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$\begin{figure} \par\includegraphics[width=5.5cm,height=7.9cm,angle=90,clip]{7141... ...includegraphics[width=5.5cm,height=7.7cm,angle=90,clip]{7141f6b.eps}\end{figure}$	Figure 6: The same as in Fig. 4, but for the spectral range $\lambda \lambda 6141$ -6172 Å ( left panels) and $\lambda \lambda 5521$ -5559 Å ( right panels).
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$\begin{figure} \par\includegraphics[angle=90,width=7.3cm,clip]{7141f7a.eps}\hspace*{4mm} \includegraphics[angle=90,width=7.3cm,clip]{7141f7b.eps}\end{figure}$	Figure 7: The same as in Fig. 4, but for the spectral range $\lambda \lambda 6099$ -6135 Å ( left panels) and $\lambda \lambda 6426$ -6454 Å ( right panels).
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$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{7141f8.eps}\end{figure}$	Figure 8: The same as in Fig. 4, but for the spectral range $\lambda \lambda 6690$ -6760 Å.
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