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$\begin{figure} \par\includegraphics[height=9.8cm,width=8.3cm,clip]{0248fig1.eps}\end{figure}$ Figure 1: Upper panel: evolution of the nuclear shells (hatched) and convective layers (shaded) in an initially metal-free model for HE 0107-5240 of $0.82~M_\odot$ during and after the core helium flash, illustrating the flash-induced mixing. The dashed line denotes the maximum of H-burning via pp-chains, the solid one that via CNO-cycle. The lower solid line is the maximum of He-burning. The hatched shells cover those regions where the energy generation is larger than 0.001 of the maximum in that particular shell, denoted by the corresponding line. Lower panel: total luminosity (dotted) and those from He-burning (solid) and H-burning (dashed). Time is in years since $\log L_{{\rm He}}/L_\odot \geq 6$ , i.e. since the He-flash has fully started.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=7.7cm,clip]{0248fig2.ps}\end{figure}$ Figure 2: Evolution of model M 2 ( $\log g$ vs. $\log T_{{\rm eff}}$ ), which is a star of $0.81~M_\odot$ and initial iron abundance of ${\rm [Fe/H]}=-5.3$ (see text for details). The error cross marks the position of HE 0107-5240.
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In the text

$\begin{figure} \par\includegraphics[height=8.4cm,width=7.8cm,clip]{0248fig3.ps}\end{figure}$ Figure 3: Evolution of our model for CS22957-027 (Table 3; solid line) compared to that of a Pop. III model similar to M1 ( $0.82~M_\odot$ ; dashed) experiencing the flash-induced mixing at the tip of the first RGB and one of a $1~M_\odot$ star of typical Pop. I composition (dash-dotted line).
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=7.7cm,clip]{0248fig2.ps}\end{figure}$	Figure 2: Evolution of model M 2 ( $\log g$ vs. $\log T_{{\rm eff}}$ ), which is a star of $0.81~M_\odot$ and initial iron abundance of ${\rm [Fe/H]}=-5.3$ (see text for details). The error cross marks the position of HE 0107-5240.
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$\begin{figure} \par\includegraphics[height=8.4cm,width=7.8cm,clip]{0248fig3.ps}\end{figure}$	Figure 3: Evolution of our model for CS22957-027 (Table 3; solid line) compared to that of a Pop. III model similar to M1 ( $0.82~M_\odot$ ; dashed) experiencing the flash-induced mixing at the tip of the first RGB and one of a $1~M_\odot$ star of typical Pop. I composition (dash-dotted line).
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