All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3002f1.ps} \end{figure}$ Figure 1: 2-28 keV light curves of the three WFC-detected bursts at varying time resolution. Typical error bars are indicated at the left and right of each panel.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{3002f2.ps} \end{figure}$ Figure 2: 2-28 keV light curve of the long burst, zooming in at low flux levels and with a time resolution of 30 s. The dotted line indicates the out-of-burst persistent flux level. There are no data during times between the two panels.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.2cm,clip]{3002f3.ps} \end{figure}$ Figure 3: 2-28 keV light curve of the long burst at a time resolution of 0.25 s, zooming in on the period of strong variability.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3002f4.ps} \end{figure}$ Figure 4: a) Time history of observed photon flux. b) Bolometric flux of modeled black body radiation. c) Color temperature of black body radiation. d) Sphere-equivalent radius of bb radiation for a distance of 5 kpc (the first data point of $208\pm 25$ km is outside the plot borders). e) $\chi ^2_\nu$ of fits. The vertical lines indicate time intervals for further spectroscopy of the dip (see Fig. 5).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3002f5.ps} \end{figure}$ Figure 5: Spectra of the 71 s lower-flux interval (lower spectrum; first interval between vertical lines in Fig. 4) and the 41 s interval after the dip (upper spectrum; last interval in Fig. 4). The crosses indicate the measurements (vertical lengths indicate 1 $\sigma$ error intervals; histograms indicate the fitted model with free $N_{\rm H}$ and fixed radius).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3002f6.ps} \end{figure}$ Figure 6: RXTE/ASM 2-12 keV light curve with a bin time of 14 d and eliminating all data points from SSC3 or with an error in excess of 0.15 c s^-1. The vertical lines in the top indicate the times when bursts were detected (solid lines WFC, dashed lines RXTE PCA (1st and last) and ASM).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{3002f7.ps} \end{figure}$ Figure 7: Top panel: from left to right LECS, MECS and PDS spectrum (crosses with vertical lines depicting 1 $\sigma$ error bars) and best fit result for power law and black body model (histogram). Bottom panel: fit residuals.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3002f8.ps} \end{figure}$ Figure 8: Ignition thicknesses and flash energies as a function of heat flux.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3002f9.ps} \end{figure}$ Figure 9: Comparison of the observed decay of the bolometric black body flux (histogram) with a theoretical model (Cumming & Macbeth 2004) for the cooling rate of a column of depth $7\times 10^{9}$ g cm^-2 and a nuclear energy release of $1.6\times 10^{18}$ erg g^-1 which is expected for helium burning to iron (dashed curve). To illustrate the dependence on these two parameters a model is shown with the same energy output (10⁴¹ erg) but for a column depth of $1\times 10^{10}$ g cm^-2and an energy release of $1.0\times 10^{18}$ erg g^-1(dashed-dotted curve).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3002f10.ps} \end{figure}$ Figure 10: Three structure plots for different moments in the evolution of a 1.5 $M_\odot$ model. Only the central 0.7 $M_\odot$ is shown, as a function of the mass coordinate. Upper panel a): Logarithm of the mass density. Middle panel b): Logarithm of the hydrogen (solid lines) and helium (dashed lines) mass fraction . Lower panel c): Logarithm of the oxygen (solid lines) and neon (dashed lines) mass fraction. The symbols on the lines indicate the model, as shown in the upper panel.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3002f1.ps} \end{figure}$	Figure 1: 2-28 keV light curves of the three WFC-detected bursts at varying time resolution. Typical error bars are indicated at the left and right of each panel.
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$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{3002f2.ps} \end{figure}$	Figure 2: 2-28 keV light curve of the long burst, zooming in at low flux levels and with a time resolution of 30 s. The dotted line indicates the out-of-burst persistent flux level. There are no data during times between the two panels.
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$\begin{figure} \par\includegraphics[angle=90,width=7.2cm,clip]{3002f3.ps} \end{figure}$	Figure 3: 2-28 keV light curve of the long burst at a time resolution of 0.25 s, zooming in on the period of strong variability.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3002f5.ps} \end{figure}$	Figure 5: Spectra of the 71 s lower-flux interval (lower spectrum; first interval between vertical lines in Fig. 4) and the 41 s interval after the dip (upper spectrum; last interval in Fig. 4). The crosses indicate the measurements (vertical lengths indicate 1 $\sigma$ error intervals; histograms indicate the fitted model with free $N_{\rm H}$ and fixed radius).
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3002f6.ps} \end{figure}$	Figure 6: RXTE/ASM 2-12 keV light curve with a bin time of 14 d and eliminating all data points from SSC3 or with an error in excess of 0.15 c s^-1. The vertical lines in the top indicate the times when bursts were detected (solid lines WFC, dashed lines RXTE PCA (1st and last) and ASM).
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$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{3002f7.ps} \end{figure}$	Figure 7: Top panel: from left to right LECS, MECS and PDS spectrum (crosses with vertical lines depicting 1 $\sigma$ error bars) and best fit result for power law and black body model (histogram). Bottom panel: fit residuals.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3002f8.ps} \end{figure}$	Figure 8: Ignition thicknesses and flash energies as a function of heat flux.
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