All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F1.eps} \end{figure}$ Figure 1: The observed CM diagram of 47 Tuc (Sosin et al. 1996) with superimposed 10 Gyr isochrones with Z=0.004 Y=0.238 (solid line) and Z=0.008 Y=0.25 (long dashed line), as evaluated by adopting a mixing lenght parameter $\alpha =1.9$ . Two horizontal branch models, corresponding to the Z=0.004 isochrone, are also shown, together with the predicted Asymptotic Giant Branch (AGB) bottom luminosity (arrow). Color transformations are from Castelli (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F2.eps} \end{figure}$ Figure 2: The evolutionary path of a 4.0 $M_{\odot }$ model (Z=0.004Y=0.238) as computed without mass loss ( $\eta =0$ , solid line) or, top to bottom, for $\eta = 2$ , 5, 8.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F3.eps} \end{figure}$ Figure 3: Evolutionary path in the log( $L/L_{\odot }$ ), log $T_{\rm e} \ {\rm [^o K]}$ diagram of the models computed for Z=0.004 Y=0.238 and the labelled mass values.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F4.eps} \end{figure}$ Figure 4: The behavior of selected masses close to $M_{\rm up}$ in the $\log T~{\rm [^o K]}$ versus $\log \rho_{\rm c}$ [g/cm³] plane for Z=0.004Y=0.238. The figure shows the behavior of the central temperature (solid line) and of the maximum temperature (dashed line) as a function of central density.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{H4256F5.eps} \end{figure}$ Figure 5: Isochrones for Z=0.004 Y=0.238 and the labeled ages.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{H4256F6a.eps}\hspace*{4mm} \includegraphics[width=8.6cm,clip]{H4256F6b.eps} \end{figure}$ Figure 6: Left panel: comparison between a 0.8 $M_{\odot }$ (Z=0.004 Y=0.24) by Girardi et al. (2000) and by the present paper with the same characteristics (no diffusion, $\alpha =1.68$ ). Right panel: comparison among our standard 0.8 $M_{\odot }$ (Z=0.004 Y=0.238) and 0.8 $M_{\odot }$ models with different characteristics (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F7.eps} \end{figure}$ Figure 7: Comparison between a 4.0 $M_{\odot }$ (Z=0.004 Y=0.238) by Girardi et al. (2000) (solid line) and by the present paper with the same characteristics (mild overshooting, $\beta =0.25$ , and $\alpha =1.68$ , dot-dashed line line). Models with $\beta =0.1$ (dashed line) and without overshooting (dotted line) are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F8.eps} \end{figure}$ Figure 8: The $\Delta M_{V}$ parameter as a function of the cluster age for the labelled assumptions about the original chemical composition and the efficiency of core overshooting (NO = canonical models). For ages larger than 5 Gyr convective cores vanish and the usual luminosity difference between HB and TO has been reported.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F2.eps} \end{figure}$	Figure 2: The evolutionary path of a 4.0 $M_{\odot }$ model (Z=0.004Y=0.238) as computed without mass loss ( $\eta =0$ , solid line) or, top to bottom, for $\eta = 2$ , 5, 8.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F3.eps} \end{figure}$	Figure 3: Evolutionary path in the log( $L/L_{\odot }$ ), log $T_{\rm e} \ {\rm [^o K]}$ diagram of the models computed for Z=0.004 Y=0.238 and the labelled mass values.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F4.eps} \end{figure}$	Figure 4: The behavior of selected masses close to $M_{\rm up}$ in the $\log T~{\rm [^o K]}$ versus $\log \rho_{\rm c}$ [g/cm³] plane for Z=0.004Y=0.238. The figure shows the behavior of the central temperature (solid line) and of the maximum temperature (dashed line) as a function of central density.
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$\begin{figure} \par\includegraphics[width=8.8cm]{H4256F5.eps} \end{figure}$	Figure 5: Isochrones for Z=0.004 Y=0.238 and the labeled ages.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{H4256F6a.eps}\hspace*{4mm} \includegraphics[width=8.6cm,clip]{H4256F6b.eps} \end{figure}$	Figure 6: Left panel: comparison between a 0.8 $M_{\odot }$ (Z=0.004 Y=0.24) by Girardi et al. (2000) and by the present paper with the same characteristics (no diffusion, $\alpha =1.68$ ). Right panel: comparison among our standard 0.8 $M_{\odot }$ (Z=0.004 Y=0.238) and 0.8 $M_{\odot }$ models with different characteristics (see text).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F7.eps} \end{figure}$	Figure 7: Comparison between a 4.0 $M_{\odot }$ (Z=0.004 Y=0.238) by Girardi et al. (2000) (solid line) and by the present paper with the same characteristics (mild overshooting, $\beta =0.25$ , and $\alpha =1.68$ , dot-dashed line line). Models with $\beta =0.1$ (dashed line) and without overshooting (dotted line) are also shown.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4256F8.eps} \end{figure}$	Figure 8: The $\Delta M_{V}$ parameter as a function of the cluster age for the labelled assumptions about the original chemical composition and the efficiency of core overshooting (NO = canonical models). For ages larger than 5 Gyr convective cores vanish and the usual luminosity difference between HB and TO has been reported.
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