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$\begin{figure} \par\includegraphics[width=1\columnwidth,clip]{f1_3560.ps}\end{figure}$ Figure 1: a) Combined EPIC pn/ MOS X-ray light curves of V1309 Ori observed with XMM-Newton in March 2001. b) Same as a) but enlarged in count rate space to emphasise the emission components during the faint phase and in the 1-8 keV hard X-ray band (red line). c) 0.1-2.4 keV X-ray light curve of V1309 Ori obtained with the ROSAT satellite at various epochs. d) UV light curve from the optical monitor onboard XMM-Newton taken with the UVW2 filter. Fluxes are given in units of 10^-15 erg cm^-2 s^-1 Å^-1 .
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In the text

$\begin{figure} \par\includegraphics[width=12.3cm,clip=,angle=-90]{f2_3560.ps}\end{figure}$ Figure 2: 0.18-8 keV EPIC pn count rates during three subsequent bright-phase intervals ( $\phi _{\rm orb}$ = 0.45-0.66) of V1309 Ori binned at a time resolution of 3 s.
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In the text

$\begin{figure} \par\includegraphics[clip=,angle=-90,width=8.5cm]{f3_3560.ps}\end{figure}$ Figure 3: Auto-correlation function of the bright-phase light curve. Time delay bins are 3 s.
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In the text

$\begin{figure} \par\includegraphics[clip=,width=8.5cm,angle=-90]{f4_3560.ps}\par\end{figure}$ Figure 4: a) EPIC pn/ MOS X-ray eclipse light curve of V1309 Ori binned at a time resolution of 240 s and b) optical light curve obtained with the 70-cm reflector of the AIP shown for comparison. The vertical lines mark the orbital phases of the white dwarf ingress/egress measured from UV HST light curves (Staude et al. 2001).
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In the text

$\begin{figure} \par\includegraphics[clip=,width=8.6cm]{f5_3560.ps}\par\end{figure}$ Figure 5: EPIC pn spectra of V1309 Ori taken during bright and faint phase, together with likely model spectra and their residua. The model of the faint phase spectrum is a 3-temperature mekal fit. The bright phase spectrum shown here includes piled-up photons, while the fit to the data uses fixed parameters derived from the pile-up free spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=12.3cm,clip=,angle=-90]{f2_3560.ps}\end{figure}$	Figure 2: 0.18-8 keV EPIC pn count rates during three subsequent bright-phase intervals ( $\phi _{\rm orb}$ = 0.45-0.66) of V1309 Ori binned at a time resolution of 3 s.
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$\begin{figure} \par\includegraphics[clip=,angle=-90,width=8.5cm]{f3_3560.ps}\end{figure}$	Figure 3: Auto-correlation function of the bright-phase light curve. Time delay bins are 3 s.
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$\begin{figure} \par\includegraphics[clip=,width=8.5cm,angle=-90]{f4_3560.ps}\par\end{figure}$	Figure 4: a) EPIC pn/ MOS X-ray eclipse light curve of V1309 Ori binned at a time resolution of 240 s and b) optical light curve obtained with the 70-cm reflector of the AIP shown for comparison. The vertical lines mark the orbital phases of the white dwarf ingress/egress measured from UV HST light curves (Staude et al. 2001).
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$\begin{figure} \par\includegraphics[clip=,width=8.6cm]{f5_3560.ps}\par\end{figure}$	Figure 5: EPIC pn spectra of V1309 Ori taken during bright and faint phase, together with likely model spectra and their residua. The model of the faint phase spectrum is a 3-temperature mekal fit. The bright phase spectrum shown here includes piled-up photons, while the fit to the data uses fixed parameters derived from the pile-up free spectrum.
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