All Figures

$\begin{figure} \par\includegraphics[width=17.55cm,clip]{3464fig1.eps} \end{figure}$ Figure 1: Light curves of the variables of our survey, except those stars already discussed in Lebzelter et al. (2005). Fourier fits with up to two periods are shown. Note that both axis scales vary from star to star. For A19, LW5, LW7, LW13 and LW14, a break has been introduced into the time axis for a better presentation of the light change. Errors on data points before JD2452700 are estimated to be 0.013 mag (Mount Stromlo data) while after this date the errors are estimated to be 0.007 mag (CTIO data).
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In the text

$\begin{figure} \par\includegraphics[width=16.3cm,clip]{3464fig2.eps} \end{figure}$ Figure 2: Light curves versus phases for selected, monoperiodic variables from Table 1. The period given in the table was used to calculate the phase.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3464fig3.eps} \end{figure}$ Figure 3: Colour-magnitude diagram of 47 Tuc. Variable stars are indicated by open circles. Asterisks mark stars taken from Fox (1982) while the triangle is V3 using data from Eggen (1975). For all variables mean magnitudes and colours were used.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3464fig4.eps} \end{figure}$ Figure 4: The K- $\log P$ diagram for the LPVs in 47 Tuc. The error bars are scaled V light amplitudes. Only variables with reasonably well-determined periods (periods without a following colon in Table 1) are shown. The lines show the sequences of LPVs in the LMC as given by Ita et al. (2004). Sequence C is thought to be linked to fundamental mode pulsation, the other sequences to first to third overtone pulsation.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3464fig5.eps} \end{figure}$ Figure 5: The tip of the 47 Tuc giant branch in the HR-diagram. K and J-K of the variables were converted to log L/ $L_{\odot }$ and $\log T_{\rm eff}$ using the transforms in Houdashelt et al. (2000a,b). The fiducial giant branch given by Hesser et al. (1987) is also shown, with V and B-V also converted to log L/ $L_{\odot }$ and $\log T_{\rm eff}$ using the transforms in Houdashelt et al. The pulsation models are plotted using symbols identified on the figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3464fig6.eps} \end{figure}$ Figure 6: The K- $\log P$ diagram for models both with and without mass loss. The fundamental mode and the first three overtones are shown. The variables with reasonably well-determined periods are also shown, as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3464fig7.eps} \end{figure}$ Figure 7: Luminosity L, pulsation period P and radii of several mass points plotted against time in a model with M = 0.6567 $M_{\odot }$ and L = 3162 $L_{\odot }$ . The linear pulsation period of this model is 240 days while the nonlinear pulsation period after 67 years of relaxation is 185 days.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3464fig8.eps} \end{figure}$ Figure 8: The growth rate $\omega _{\rm r}$ (days^-1 plotted against log L/ $L_{\odot }$ for the models in the mass loss sequence. $\omega _{\rm r}$ is the real part of the eigenvalue $\omega$ where a time dependence exp( $\omega t$ ) is assumed. The K magnitude for AGB stars is shown on the top axis.
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In the text

$\begin{figure} \par\includegraphics[width=16.3cm,clip]{3464fig2.eps} \end{figure}$	Figure 2: Light curves versus phases for selected, monoperiodic variables from Table 1. The period given in the table was used to calculate the phase.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3464fig3.eps} \end{figure}$	Figure 3: Colour-magnitude diagram of 47 Tuc. Variable stars are indicated by open circles. Asterisks mark stars taken from Fox (1982) while the triangle is V3 using data from Eggen (1975). For all variables mean magnitudes and colours were used.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3464fig6.eps} \end{figure}$	Figure 6: The K- $\log P$ diagram for models both with and without mass loss. The fundamental mode and the first three overtones are shown. The variables with reasonably well-determined periods are also shown, as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3464fig7.eps} \end{figure}$	Figure 7: Luminosity L, pulsation period P and radii of several mass points plotted against time in a model with M = 0.6567 $M_{\odot }$ and L = 3162 $L_{\odot }$ . The linear pulsation period of this model is 240 days while the nonlinear pulsation period after 67 years of relaxation is 185 days.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3464fig8.eps} \end{figure}$	Figure 8: The growth rate $\omega _{\rm r}$ (days^-1 plotted against log L/ $L_{\odot }$ for the models in the mass loss sequence. $\omega _{\rm r}$ is the real part of the eigenvalue $\omega$ where a time dependence exp( $\omega t$ ) is assumed. The K magnitude for AGB stars is shown on the top axis.
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