All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0281fig1.ps} \end{figure}$ Figure 1: rms scatter in equivalent width differences $\Delta$ EW between the components of the binaries analyzed in this paper as a function of temperature difference $\Delta T_{{\rm eff}}$ . Open circles represent stars with rotational broadening larger than about 5 km s^-1, filled circles slowly rotating stars, asterisks the two pairs with slightly evolved primaries.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{0281fig2.ps} \end{figure}$ Figure 2: Color-Magnitude diagram for primaries using Hipparcos and Tycho magnitudes (corrected to the standard system using Bessell 2000) with Hipparcos parallaxes and our spectroscopically determined effective temperatures. The solar metallicity isochrones by Girardi et al. (2002) are overplotted for ages of 1, 2.5, 4 and 8 Gyr.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0281fig3.ps} \end{figure}$ Figure 3: Microturbulence as a function of effective temperature resulting from the analysis performed leaving the microturbulence as a free parameter. Symbols as in Fig. 1. The relation between temperature and microturbulence adopted in the analysis is shown as a continuous line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0281fig4.ps} \end{figure}$ Figure 4: Iron abundance derived for each line for the components of HIP 104687A 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.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0281fig5.ps} \end{figure}$ Figure 5: Differences between the temperatures derived using the iron and vanadium lines as a function of the temperature of the secondary.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0281fig6.ps} \end{figure}$ Figure 6: Magnitude vs. temperature differences. The dotted line represents the typical slope alone the main sequence of a 1 Gyr solar metallicity isochrone. Symbols as in Fig. 1. The two discrepant cases are HD 135101 and HD 19440, that have primaries clearly evolved off of the main sequence.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0281fig7.ps} \end{figure}$ Figure 7: Iron abundance difference between the components of pairs as a function of temperature difference. Open circles represent stars with rotation broadening larger than about 5 km s^-1, filled circles slowly rotating stars.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0281fig8.ps} \end{figure}$ Figure 8: Iron abundance difference between the components of pairs as a function effective temperature of the primary. Open and filled circles as in Fig. 7.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0281fig9.ps} \end{figure}$ Figure 9: Iron abundance difference between the components of pairs as a function effective temperature of the secondary. Open and filled circles as in Fig. 7.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0281fig10.ps} \end{figure}$ Figure 10: Estimate of iron accreted by the metal-rich component of each pair as a function of its effective temperature, taking into account the mass of the mixing zone as in Murray et al. (2001). Open and filled circles as in Fig. 7. The mass of meteoritic material is about 5.5 times the mass of iron.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0281fig1.ps} \end{figure}$	Figure 1: rms scatter in equivalent width differences $\Delta$ EW between the components of the binaries analyzed in this paper as a function of temperature difference $\Delta T_{{\rm eff}}$ . Open circles represent stars with rotational broadening larger than about 5 km s^-1, filled circles slowly rotating stars, asterisks the two pairs with slightly evolved primaries.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{0281fig2.ps} \end{figure}$	Figure 2: Color-Magnitude diagram for primaries using Hipparcos and Tycho magnitudes (corrected to the standard system using Bessell 2000) with Hipparcos parallaxes and our spectroscopically determined effective temperatures. The solar metallicity isochrones by Girardi et al. (2002) are overplotted for ages of 1, 2.5, 4 and 8 Gyr.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0281fig3.ps} \end{figure}$	Figure 3: Microturbulence as a function of effective temperature resulting from the analysis performed leaving the microturbulence as a free parameter. Symbols as in Fig. 1. The relation between temperature and microturbulence adopted in the analysis is shown as a continuous line.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0281fig4.ps} \end{figure}$	Figure 4: Iron abundance derived for each line for the components of HIP 104687A 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.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0281fig5.ps} \end{figure}$	Figure 5: Differences between the temperatures derived using the iron and vanadium lines as a function of the temperature of the secondary.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0281fig6.ps} \end{figure}$	Figure 6: Magnitude vs. temperature differences. The dotted line represents the typical slope alone the main sequence of a 1 Gyr solar metallicity isochrone. Symbols as in Fig. 1. The two discrepant cases are HD 135101 and HD 19440, that have primaries clearly evolved off of the main sequence.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0281fig7.ps} \end{figure}$	Figure 7: Iron abundance difference between the components of pairs as a function of temperature difference. Open circles represent stars with rotation broadening larger than about 5 km s^-1, filled circles slowly rotating stars.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0281fig8.ps} \end{figure}$	Figure 8: Iron abundance difference between the components of pairs as a function effective temperature of the primary. Open and filled circles as in Fig. 7.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0281fig9.ps} \end{figure}$	Figure 9: Iron abundance difference between the components of pairs as a function effective temperature of the secondary. Open and filled circles as in Fig. 7.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{0281fig10.ps} \end{figure}$	Figure 10: Estimate of iron accreted by the metal-rich component of each pair as a function of its effective temperature, taking into account the mass of the mixing zone as in Murray et al. (2001). Open and filled circles as in Fig. 7. The mass of meteoritic material is about 5.5 times the mass of iron.
Open with DEXTER