All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3390fig1.eps} \end{figure}$ Figure 1: Global evolution of one of our models from the ZAMS into the early AGB. The sense of evolution from the RGB-tip through the HB and up to the early AGB is indicated by arrows. The location of the ZAHB corresponds to the point labeled A. Note that HB evolution is initially bluewards, as shown by the arrows.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3390fig2.eps} \end{figure}$ Figure 2: Evolution of the total, H- and He-burning luminosities for the model shown in Fig. 1 from the onset of the He-core flash until the model has settled on the HB. The moment when the ZAHB is reached is indicated with a vertical dashed line and corresponds to $1.325\times 10^6$ yr after the onset of the flash.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3390fig3.eps} \end{figure}$ Figure 3: Horizontal branch evolution for models evolved from the main sequence but with different Reimers mass loss parameter $\eta$ as indicated in the figure. Initial mass and composition are the same as for the model of Fig. 1. We show only the part starting at the ZAHB, which is indicated by a star.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{3390fig4.eps} \end{figure}$ Figure 4: Comparison between full and approximate models constructed with methods M1, M2 and M3 for a typical cool (red) HB stellar model. Top panel: evolution in the HRD, starting with the ZAHB and up to the early AGB. The characteristics of the progenitor and the mass of the model on the HB are indicated, as well as the meaning of the different linetypes. The asterisk denotes the point where the central helium mass fraction drops below 0.01 in the full model (in the scale of this plot, however, equivalent points in all sequences overlap almost completely). Middle panels: luminosity and relative luminosity differences for approximate models with respect to the full model against time. Indices f and Mi indicate full models respectively the i-th method. Bottom panels: effective temperature and relative effective temperature differences against time. Ages are counted from the ZAHB. Middle and lower panels show the evolution until the end of the HB evolution only, defined by the end of core helium burning.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{3390fig5.eps} \end{figure}$ Figure 5: The same as Fig. 4 but for a typical intermediate HB model. Characteristics of the model are given in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3390fig6.eps} \end{figure}$ Figure 6: The same as Fig. 4 but for a typical hot HB model. Characteristics of the model are given in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3390fig1.eps} \end{figure}$	Figure 1: Global evolution of one of our models from the ZAMS into the early AGB. The sense of evolution from the RGB-tip through the HB and up to the early AGB is indicated by arrows. The location of the ZAHB corresponds to the point labeled A. Note that HB evolution is initially bluewards, as shown by the arrows.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3390fig2.eps} \end{figure}$	Figure 2: Evolution of the total, H- and He-burning luminosities for the model shown in Fig. 1 from the onset of the He-core flash until the model has settled on the HB. The moment when the ZAHB is reached is indicated with a vertical dashed line and corresponds to $1.325\times 10^6$ yr after the onset of the flash.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3390fig3.eps} \end{figure}$	Figure 3: Horizontal branch evolution for models evolved from the main sequence but with different Reimers mass loss parameter $\eta$ as indicated in the figure. Initial mass and composition are the same as for the model of Fig. 1. We show only the part starting at the ZAHB, which is indicated by a star.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{3390fig5.eps} \end{figure}$	Figure 5: The same as Fig. 4 but for a typical intermediate HB model. Characteristics of the model are given in the top panel.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3390fig6.eps} \end{figure}$	Figure 6: The same as Fig. 4 but for a typical hot HB model. Characteristics of the model are given in the top panel.
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