All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4896fig1.ps} \end{figure}$ Figure 1: The rms scatter in equivalent-width differences $\Delta {\it EW}$ between the components of the binaries analyzed in this paper as a function of temperature difference $\Delta T_{\rm eff}$ . Open circles represent pairs with a temperature difference larger than 400 K, and the primary clearly evolved off the main sequence and active stars. Filled circles represent the other pairs. The anomalously large scatter in EW difference for HIP 64030 (plotted as an open square) is probably due to the large abundance difference between the components.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4896fg2a.ps}\par\vspace*{2mm} \includegraphics[width=7.8cm,clip]{4896fg2b.ps} \end{figure}$ Figure 2: Comparison of SARG and FEROS EWs. Upper panel: run 1 (August 2001); lower panel: run 2 (March 2002).
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{4896fg3a.ps}\par\vspace*{2... ...par\vspace*{2mm} \includegraphics[width=6.7cm,clip]{4896fg3e.ps} \end{figure}$ Figure 3: Position of the components of the pairs for which Hipparcos parallaxes yielded inconsistent position in the HR diagram ( left panel) and in the $T_{\rm eff} - \log g$ diagram ( right panel). Open circles: results of abundance analysis performed adopting the Hipparcos distance; filled circles: adopting spectroscopic distances. Isochrones by Girardi et al. (2002) of suitable ages and metallicties are overplotted. From top to bottom: HIP 3290, HIP 55288; HIP 58864/2; HIP 76603/2, HIP 79818.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4896fig4.ps} \end{figure}$ Figure 4: Iron abundance derived for each line of the components of HIP 114914 A and B. A clear correlation is present, indicating that the use of a line-by-line differential analysis significantly reduces the errors on abundance difference between the components.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fig5.ps} \end{figure}$ Figure 5: Difference between the temperature differences based on Fe and V lines as a function of the temperature of the secondary. Symbols as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fig6.ps} \end{figure}$ Figure 6: Magnitude vs. temperature differences. The dotted line represents the typical slope along the main sequence of a 1 Gyr solar-metallicity isochrone. Symbols as in Fig. 1. The three stars clearly above the mean relation are HIP 3290, HIP 74332, and HIP 80399, which all have primaries evolved off of the main sequence. The pair with a magnitude difference that is too small for the measured temperature difference is HIP 103438.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fig7.ps} \end{figure}$ Figure 7: Iron abundance difference between the components of pairs as a function of the temperature difference. Symbols as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg8a.ps}\par\vspace*{2mm} \includegraphics[width=8.4cm,clip]{4896fg8b.ps} \end{figure}$ Figure 8: Iron abundance difference between the components of pairs as a function of the effective temperature of the primary ( upper panel) and the secondary ( lower panel). Symbols as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fig9.ps} \end{figure}$ Figure 9: Iron abundance of the primary between the components of pairs as a function of the metallicity of the primary. Symbols as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg10.ps} \end{figure}$ Figure 10: Estimate of the effect of errors on the absolute magnitude on the differential analysis for pairs as a function of the temperature difference between the components. The abscissa shows the slope of the variation in abundance difference between the components of the pairs as a function of the absolute distance modulus (dex/mag).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4896fg11.ps} \end{figure}$ Figure 11: Abundance difference of HIP 64030 as a function of EW ( upper panel), EP ( middle panel) and wavelength ( lower panel). No clear trends are present.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg12.ps} \end{figure}$ Figure 12: Position of the components of HIP 64030 in the HR diagram ( left panel) and in the $T_{\rm eff} - \log g$ diagram ( right panel). Open circles: results of abundance analysis performed when adopting the Hipparcos distance; filled circles: when adopting spectroscopic distances. Isochrones by Girardi et al. (2002) are overplotted.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg13.ps} \end{figure}$ Figure 13: Abundance difference of HIP 76602/3 as a function of EW ( upper panel), EP ( middle panel), and wavelength ( lower panel). No clear trends are present.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg14.ps} \end{figure}$ Figure 14: Position of the components of HIP 80399 in the HR diagram ( left panel) and in the $T_{\rm eff} - \log g$ diagram, using absolute magnitude from Hipparcos parallaxes and effective temperature and gravities from our analysis. Overplotted are the 1, 2.5, 4.0 and 6.3 Gyr isochrones of solar composition by Girardi et al. (2002).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg15.ps} \end{figure}$ Figure 15: Estimate of iron accreted by the metal-rich component of each pair as a function of its effective temperature, taking the mass of the mixing zone into account as in Murray et al. (2001). Symbols as in Fig. 7. The mass of meteoritic material is about 5.5 times the mass of iron.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg16.ps} \end{figure}$ Figure 16: Estimate of iron accreted by the metal-rich component of each pair as a function of its effective temperature for the pairs studied in this paper and in Paper I. The horizontal lines show the amount of iron expected to have been accreted by the Sun during the main sequence lifetime ( $0.4~M_{\oplus}$ , Murray et al. 2001) and the amount of iron corresponding to the upper limit on abundance difference between the inner and outer regions of the Sun according to helioseismology ( $2~M_{\oplus}$ , Winnick et al. 2002). The mass of meteoritic material is assumed to be about 5.5 times the mass of iron.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4896fg2a.ps}\par\vspace*{2mm} \includegraphics[width=7.8cm,clip]{4896fg2b.ps} \end{figure}$	Figure 2: Comparison of SARG and FEROS EWs. Upper panel: run 1 (August 2001); lower panel: run 2 (March 2002).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4896fig4.ps} \end{figure}$	Figure 4: Iron abundance derived for each line of the components of HIP 114914 A and B. A clear correlation is present, indicating that the use of a line-by-line differential analysis significantly reduces the errors on abundance difference between the components.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fig5.ps} \end{figure}$	Figure 5: Difference between the temperature differences based on Fe and V lines as a function of the temperature of the secondary. Symbols as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fig7.ps} \end{figure}$	Figure 7: Iron abundance difference between the components of pairs as a function of the temperature difference. Symbols as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg8a.ps}\par\vspace*{2mm} \includegraphics[width=8.4cm,clip]{4896fg8b.ps} \end{figure}$	Figure 8: Iron abundance difference between the components of pairs as a function of the effective temperature of the primary ( upper panel) and the secondary ( lower panel). Symbols as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fig9.ps} \end{figure}$	Figure 9: Iron abundance of the primary between the components of pairs as a function of the metallicity of the primary. Symbols as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg10.ps} \end{figure}$	Figure 10: Estimate of the effect of errors on the absolute magnitude on the differential analysis for pairs as a function of the temperature difference between the components. The abscissa shows the slope of the variation in abundance difference between the components of the pairs as a function of the absolute distance modulus (dex/mag).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4896fg11.ps} \end{figure}$	Figure 11: Abundance difference of HIP 64030 as a function of EW ( upper panel), EP ( middle panel) and wavelength ( lower panel). No clear trends are present.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg12.ps} \end{figure}$	Figure 12: Position of the components of HIP 64030 in the HR diagram ( left panel) and in the $T_{\rm eff} - \log g$ diagram ( right panel). Open circles: results of abundance analysis performed when adopting the Hipparcos distance; filled circles: when adopting spectroscopic distances. Isochrones by Girardi et al. (2002) are overplotted.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg13.ps} \end{figure}$	Figure 13: Abundance difference of HIP 76602/3 as a function of EW ( upper panel), EP ( middle panel), and wavelength ( lower panel). No clear trends are present.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg14.ps} \end{figure}$	Figure 14: Position of the components of HIP 80399 in the HR diagram ( left panel) and in the $T_{\rm eff} - \log g$ diagram, using absolute magnitude from Hipparcos parallaxes and effective temperature and gravities from our analysis. Overplotted are the 1, 2.5, 4.0 and 6.3 Gyr isochrones of solar composition by Girardi et al. (2002).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4896fg15.ps} \end{figure}$	Figure 15: Estimate of iron accreted by the metal-rich component of each pair as a function of its effective temperature, taking the mass of the mixing zone into account as in Murray et al. (2001). Symbols as in Fig. 7. The mass of meteoritic material is about 5.5 times the mass of iron.
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