All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{6150fig1.ps} \end{figure}$ Figure 1: 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 adopting the Hipparcos distance; filled circles: adopting spectroscopic distances. Isochrones by Salasnich et al. (2000) with Z=0.008 and [ $\alpha$ /Fe] = 0.3, close to the surface abundances of the primary, are overplotted. It is not possible to fit both components with a single isochrone. The most likely explanation is that the primary is a blue straggler.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6150fig2.ps} \end{figure}$ Figure 2: The radial velocities of HIP 64030A phased to the preliminary orbital period (445 days). The best-fit orbital solution is overplotted. Radial velocities from different sources are represented by different symbols: filled circles: SARG (this paper); filled squares: McDonald (this paper); open circle: FEROS (Desidera et al. 2006b); empty squares: CORAVEL (this paper); empty upper triangles: Struve & Zebergs (1959); upside down triangle: Andersen & Nordstrom (1985).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6150fig3.ps} \end{figure}$ Figure 3: Relative motion of HIP 64030A and B. The continuous line is the linear fitting to the data (without weighting). The dashed line is the relative motion measured by Hipparcos (extrapolated to a timescale much larger than the mission lifetime).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6150fig4.ps} \end{figure}$ Figure 4: Possible orbital parameters of the wide binary as a function of the (unknown) separation along the line of sight.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,height=9cm,clip]{6150fig5.ps} \end{figure}$ Figure 5: A portion of the spectra used to derive the C isotopic ratio using spectral synthesis. Upper panel: the comparison star HIP 69328A, central panel: HIP 64030B, lower panel: HIP 64030A.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{6150fig6.ps} \end{figure}$ Figure 6: CN spectral synthesis. Upper panel: HIP 64030B, lower panel: HIP 64030A.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6150fig7.ps} \end{figure}$ Figure 7: Li spectral synthesis. Upper panel: HIP 64030B, lower panel: HIP 64030A.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6150fig8.ps} \end{figure}$ Figure 8: Lithium abundance vs. effective temperature for the components of HIP 64030 (filled symbols) compared with those of stars in the Hyades (Thorburn et al. 1993; open circles: stars with Li detection; open squares: upper limits) and in M 67 (Jones et al. 1999; crosses: stars with Li detection; open triangles: upper limits).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6150fig9.ps} \end{figure}$ Figure 9: Abundance difference as a function of condensation temperature. Filled and empty circles represent abundance differences from neutral and single-ionized species when at least two lines are available, while crosses represent elements for which one single line is included in the analysis. Asterisks represent the elements for which abundance was obtained by spectral synthesis.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6150fg10.ps} \end{figure}$ Figure 10: Abundance difference as a function of condensation temperature. Only elements with at least two lines are plotted. Abundance difference from neutral and single-ionized species were averaged. Empty circles represent siderophiles elements, and filled circles the other elements. Siderophiles show a larger abundance difference with respect to other elements for similar condensation temperatures.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6150fg11.ps} \end{figure}$ Figure 11: Period eccentricity relation for post AGB and RV Tauri stars with depleted abundances (empty squares) and normal abundances (empty circles) from Maas (2003) and of field blue stragglers studied by Preston & Sneden (2000) and Carney et al. (2005) (asterisks). The position of HIP 64030 is overplotted as a filled circle.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6150fig3.ps} \end{figure}$	Figure 3: Relative motion of HIP 64030A and B. The continuous line is the linear fitting to the data (without weighting). The dashed line is the relative motion measured by Hipparcos (extrapolated to a timescale much larger than the mission lifetime).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6150fig4.ps} \end{figure}$	Figure 4: Possible orbital parameters of the wide binary as a function of the (unknown) separation along the line of sight.
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$\begin{figure} \par\includegraphics[width=7.2cm,height=9cm,clip]{6150fig5.ps} \end{figure}$	Figure 5: A portion of the spectra used to derive the C isotopic ratio using spectral synthesis. Upper panel: the comparison star HIP 69328A, central panel: HIP 64030B, lower panel: HIP 64030A.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{6150fig6.ps} \end{figure}$	Figure 6: CN spectral synthesis. Upper panel: HIP 64030B, lower panel: HIP 64030A.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6150fig7.ps} \end{figure}$	Figure 7: Li spectral synthesis. Upper panel: HIP 64030B, lower panel: HIP 64030A.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6150fig8.ps} \end{figure}$	Figure 8: Lithium abundance vs. effective temperature for the components of HIP 64030 (filled symbols) compared with those of stars in the Hyades (Thorburn et al. 1993; open circles: stars with Li detection; open squares: upper limits) and in M 67 (Jones et al. 1999; crosses: stars with Li detection; open triangles: upper limits).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6150fig9.ps} \end{figure}$	Figure 9: Abundance difference as a function of condensation temperature. Filled and empty circles represent abundance differences from neutral and single-ionized species when at least two lines are available, while crosses represent elements for which one single line is included in the analysis. Asterisks represent the elements for which abundance was obtained by spectral synthesis.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6150fg11.ps} \end{figure}$	Figure 11: Period eccentricity relation for post AGB and RV Tauri stars with depleted abundances (empty squares) and normal abundances (empty circles) from Maas (2003) and of field blue stragglers studied by Preston & Sneden (2000) and Carney et al. (2005) (asterisks). The position of HIP 64030 is overplotted as a filled circle.
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