All Figures

$\begin{figure} \par\mbox{\psfig{figure=H4336F1.eps,width=5.9cm,clip}\hspace*{2mm... ...m,clip}\hspace*{2mm} \psfig{figure=H4336F9.eps,width=5.6cm,clip} }\end{figure}$ Figure 1: ASM/RXTE lightcurves of 9 of the most frequent X-ray bursters in the WFC database. Each bin is a one week average. Below the lightcurve the WFC observations on these sources are indicated with horizontal bars. The arrows just above the horizontal bars indicate the times of type I bursts.
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In the text

$\begin{figure} \vspace*{4.5cm} \mbox{\epsfig{figure=H4336F10.eps,width=5.8cm,bbu... ...gure=H4336F18.eps,width=5.8cm,bburx=470,clip=t} } \vspace*{-0.5mm}\end{figure}$ Figure 2: Burst rate, $N_{\rm burst}$ , as a function of the observed count rate, $F_{\rm pers}$ (WFC cts s^-1 cm^-2; bottom axis) and the persistent flux, $F_{\rm pers}$ (10^-8 erg s^-1 cm^-2; top axis) for the nine frequent X-ray bursters in the galactic center region. The photon and energy flux are for a bandpass of 2-28 keV.
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In the text

$\begin{figure} \par\mbox{\psfig{figure=H4336F19.eps,angle=-90,width=6.2cm}\hspac... ...}\hspace*{4mm} \psfig{figure=H4336F21.eps,angle=-90,width=5.4cm} }\end{figure}$ Figure 3: The wait time, $\Delta$ Time, as a function of persistent flux, $F_{\rm pers}$ , for the sources GS 1826-24 (left panel) and KS 1731-260 (middle panel) and GX 354-0 (right panel). A typical error in the flux for GS 1826-24 is indicated at the bottom left, while the error in the flux for the other two sources is as large as a dot. The error in the wait time for all sources is much smaller than the size of a dot. A best linear fit is drawn for the bursts for which the previous burst is not missed.
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In the text

$\begin{figure} \par\mbox{\psfig{figure=H4336F22.eps,angle=-90,width=5.9cm}\hspac... ...}\hspace*{3mm} \psfig{figure=H4336F30.eps,angle=-90,width=5.6cm} }\end{figure}$ Figure 4: The exponential decay time, $\tau$ , as a function of persistent flux, F, for the nine most frequent burst sources observed with WFC. In the upper-right corner of each panel a typical error-bar is shown.
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In the text

$\begin{figure} \par\psfig{figure=H4336F31.eps,width=8.4cm,clip} \end{figure}$ Figure 5: A schematic diagram of the burst rate as a function of luminosity for the nine X-ray burst sources (see Fig. 2). Between the solid lines the region is indicated where the burst rate drops by a factor of 5. No type I bursts were observed at luminosities above the dashed line. The dotted-dashed line indicates the theoretical predicted transition from hydrogen-rich bursts to pure helium bursts.
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In the text

$\begin{figure} \par\mbox{\psfig{figure=H4336F1.eps,width=5.9cm,clip}\hspace{2mm... ...m,clip}\hspace{2mm} \psfig{figure=H4336F9.eps,width=5.6cm,clip} }\end{figure}$	Figure 1: ASM/RXTE lightcurves of 9 of the most frequent X-ray bursters in the WFC database. Each bin is a one week average. Below the lightcurve the WFC observations on these sources are indicated with horizontal bars. The arrows just above the horizontal bars indicate the times of type I bursts.
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$\begin{figure} \vspace{4.5cm} \mbox{\epsfig{figure=H4336F10.eps,width=5.8cm,bbu... ...gure=H4336F18.eps,width=5.8cm,bburx=470,clip=t} } \vspace{-0.5mm}\end{figure}$	Figure 2: Burst rate, $N_{\rm burst}$ , as a function of the observed count rate, $F_{\rm pers}$ (WFC cts s^-1 cm^-2; bottom axis) and the persistent flux, $F_{\rm pers}$ (10^-8 erg s^-1 cm^-2; top axis) for the nine frequent X-ray bursters in the galactic center region. The photon and energy flux are for a bandpass of 2-28 keV.
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$\begin{figure} \par\mbox{\psfig{figure=H4336F22.eps,angle=-90,width=5.9cm}\hspac... ...}\hspace*{3mm} \psfig{figure=H4336F30.eps,angle=-90,width=5.6cm} }\end{figure}$	Figure 4: The exponential decay time, $\tau$ , as a function of persistent flux, F, for the nine most frequent burst sources observed with WFC. In the upper-right corner of each panel a typical error-bar is shown.
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