All Figures

$\begin{figure} \par\includegraphics[height=9.7cm,width=17.5cm]{8024fig13.eps}\end{figure}$ Figure 13: The dependence of the amount of core overshooting with the logarithm of mass (in solar units). The continuous thick line (full rectangles and error bars) represents the results obtained in the present paper while dashed line (asterisks) denotes the relationship established by Ribas et al. (2000).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig1.eps} \end{figure}$ Figure 1: Mass-radius diagram for the individual components (connected by line) of the binary systems in Table 1. Theoretical isochones are also shown for reference as dashed lines. The ages are $1\times 10^6$ , $1\times 10^7$ and $1\times 10^8$ years. (X, Z) = (0.70, 0.02) and $\alpha _{\rm ov} = 0.2$ .
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig2.eps} \end{figure}$ Figure 2: The theoretical ratio of the effective temperatures TR ( upper panels), the surface grativity for the two components ( lower panels) of TZ For as a function of time. Solid lines denote the theoretical calculations while horizontal dashed lines indicate the observed values. The values of $\alpha _{\rm ov}$ are 0.0, 0.2, 0.4, and 0.6 from the left to right. (X, Z) = (0.71, 0.018).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig3.eps} \end{figure}$ Figure 3: The same as in Fig. 1 but for AI Hya. (X, Z) = (0.71, 0.02).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig4.eps} \end{figure}$ Figure 4: The same as in Fig. 1 but for YZ Cas. (X, Z) = (0.715, 0.015).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig5.eps} \end{figure}$ Figure 5: Isochrones for SZ Cen. Main frame: mass-radius diagram. Small diagram: mass of the primary star versus TR (for this figure and for V3903 Sgr, V906 Sco, WX Cep, TR is redefined to be $\equiv$ $T_{\rm eff 1}/T_{\rm eff 2}$ ). Only the case of no overshooting is shown. (X, Z) = (0.70, 0.02).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig6.eps} \end{figure}$ Figure 6: The same as in Fig. 1 but for V1031 Ori. (X, Z) = (0.71, 0.015).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig7.eps} \end{figure}$ Figure 7: The same as in Fig. 4 but for WX Cep. Only the case with $\alpha _{\rm ov} = 0.2$ is shown. (X, Z) = (0.70, 0.02).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig8.eps} \end{figure}$ Figure 8: The same as in Fig. 4 but for V906 Sco. Only the case of no overshooting is shown. (X, Z) = (0.70, 0.02).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig9.eps} \end{figure}$ Figure 9: The same as in Fig. 1 but for $\chi ^{2}$ Hya. (X, Z) = (0.71, 0.015).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig10.eps} \end{figure}$ Figure 10: The same as in Fig. 1 but for V380 Cyg. (X, Z) = (0.71, 0.015).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig11.eps} \end{figure}$ Figure 11: The same as in Fig. 1 but for V453 Cyg. (X, Z) = (0.71, 0.015).
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In the text

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig12.eps} \end{figure}$ Figure 12: The same as in Fig. 4 but for V3903 Sgr. Only models with $\alpha _{\rm ov} = 0.4$ are shown. (X, Z) = (0.70, 0.02).
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In the text

$\begin{figure} \par\includegraphics[height=9.7cm,width=17.5cm]{8024fig13.eps}\end{figure}$	Figure 13: The dependence of the amount of core overshooting with the logarithm of mass (in solar units). The continuous thick line (full rectangles and error bars) represents the results obtained in the present paper while dashed line (asterisks) denotes the relationship established by Ribas et al. (2000).
Open with DEXTER

$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig1.eps} \end{figure}$	Figure 1: Mass-radius diagram for the individual components (connected by line) of the binary systems in Table 1. Theoretical isochones are also shown for reference as dashed lines. The ages are $1\times 10^6$ , $1\times 10^7$ and $1\times 10^8$ years. (X, Z) = (0.70, 0.02) and $\alpha _{\rm ov} = 0.2$ .
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig2.eps} \end{figure}$	Figure 2: The theoretical ratio of the effective temperatures TR ( upper panels), the surface grativity for the two components ( lower panels) of TZ For as a function of time. Solid lines denote the theoretical calculations while horizontal dashed lines indicate the observed values. The values of $\alpha _{\rm ov}$ are 0.0, 0.2, 0.4, and 0.6 from the left to right. (X, Z) = (0.71, 0.018).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig3.eps} \end{figure}$	Figure 3: The same as in Fig. 1 but for AI Hya. (X, Z) = (0.71, 0.02).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig4.eps} \end{figure}$	Figure 4: The same as in Fig. 1 but for YZ Cas. (X, Z) = (0.715, 0.015).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig5.eps} \end{figure}$	Figure 5: Isochrones for SZ Cen. Main frame: mass-radius diagram. Small diagram: mass of the primary star versus TR (for this figure and for V3903 Sgr, V906 Sco, WX Cep, TR is redefined to be $\equiv$ $T_{\rm eff 1}/T_{\rm eff 2}$ ). Only the case of no overshooting is shown. (X, Z) = (0.70, 0.02).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig6.eps} \end{figure}$	Figure 6: The same as in Fig. 1 but for V1031 Ori. (X, Z) = (0.71, 0.015).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig7.eps} \end{figure}$	Figure 7: The same as in Fig. 4 but for WX Cep. Only the case with $\alpha _{\rm ov} = 0.2$ is shown. (X, Z) = (0.70, 0.02).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig8.eps} \end{figure}$	Figure 8: The same as in Fig. 4 but for V906 Sco. Only the case of no overshooting is shown. (X, Z) = (0.70, 0.02).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig9.eps} \end{figure}$	Figure 9: The same as in Fig. 1 but for $\chi ^{2}$ Hya. (X, Z) = (0.71, 0.015).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig10.eps} \end{figure}$	Figure 10: The same as in Fig. 1 but for V380 Cyg. (X, Z) = (0.71, 0.015).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig11.eps} \end{figure}$	Figure 11: The same as in Fig. 1 but for V453 Cyg. (X, Z) = (0.71, 0.015).
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$\begin{figure} \par\includegraphics[height=10.cm,width=18.cm]{8024fig12.eps} \end{figure}$	Figure 12: The same as in Fig. 4 but for V3903 Sgr. Only models with $\alpha _{\rm ov} = 0.4$ are shown. (X, Z) = (0.70, 0.02).
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