All Figures

$\begin{figure} \par\includegraphics[width=17.542cm,clip]{ms0145f1.eps} % \end{figure}$ Figure 1: Photometric observations of DW UMa. Note the much larger range of the y-axis in the upper row panel.
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In the text

$\begin{figure} \par\includegraphics*[width=8.8cm,clip]{ms0145f2.eps} \end{figure}$ Figure 2: Part of the long-term light curve of DW UMa obtained by RoboScope (Honeycutt et al. 2003) with the epochs of our observations marked with the vertical bars and the mean out-of-eclipse magnitudes shown with open squares. Our observations in 2000 have been obtained on the rising branch of a deep low state. For clarity, the RoboScope data obtained during eclipse have been removed.
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In the text

$\begin{figure} \par\includegraphics*[width=8.8cm]{ms0145f3.eps} \end{figure}$ Figure 3: Eclipse depth as a function of the out-of-eclipse magnitude of DW UMa. Filled circles - Rozhen V-band photometric observations; open circles - unfiltered observations.
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In the text

$\begin{figure} \par\includegraphics*[width=18cm,clip]{ms0145f4.eps} \end{figure}$ Figure 4: Periododgram analysis of DW UMa in 2002 - left and in 2003 - right. The insets show the mean superhump shape.
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In the text

$\begin{figure} \par\includegraphics*[width=8.8cm,clip]{ms0145f5.eps} \end{figure}$ Figure 5: Mean power spectrum of DW UMa in double logarithmic scale.
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In the text

$\begin{figure} \par\includegraphics*[width=18cm,clip]{ms0145f6.eps} \end{figure}$ Figure 6: Eclipse mapping of DW UMa. a) mean light curves with the best fits. The dotted and the dashed lines are the fits to the unfiltered high state eclipses in 2002 and 2003, respectively, overplotted on the V-band high state one; b-e) accretion disc eclipse maps, the WD's Roche lobe is shown with dotted line and the shadow of the secondary at orbital phases 0.0 and 0.041 with dashed line; f) radial intensity profiles of the accretion disc: open squares - V-band high state, filled squares - V-band intermediate state, and dotted and dashed lines - unfiltered high state in 2002 and 2003, respectively.
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In the text

$\begin{figure} \par\includegraphics*[width=12cm]{ms0145f7.eps} \end{figure}$ Figure 7: Radial profile of the AD brightness temperature obtained by using (i) temperature dependent limb-darkening coefficient - symbols connected with solid lines and (ii) with constant limb-darkening coefficient of 0.6 - symbols connected with dash-dotted lines. The dotted curves show the effective temperature of steady-state ADs for mass transfer rates $\dot{M}=10^{-10}-10^{-7}~M_\odot$ yr^-1 onto 0.77 $~M_\odot$ WD.
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In the text

$\begin{figure} \par\includegraphics*[width=18cm,clip]{ms0145f8.eps} \end{figure}$ Figure 8: Reconstruction of the radial V-band intensity profile of simulated eclipses with S/N ratio of 100. Dots - the reconstruction, solid line - the disc profile used to simulate the eclipse. a-c) Flat discs with different radial dependence of the temperature, d-f) 3D steady-state discs with emitting outer rims of different height (see text for details). In all reconstructions the eclipses were fitted to reduced $\chi ^2=1$ using a flat 1D disc geometry and full azimuthal streaming default images.
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In the text

$\begin{figure} \par\includegraphics[width=17.542cm,clip]{ms0145f1.eps} % \end{figure}$	Figure 1: Photometric observations of DW UMa. Note the much larger range of the y-axis in the upper row panel.
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$\begin{figure} \par\includegraphics*[width=8.8cm,clip]{ms0145f2.eps} \end{figure}$	Figure 2: Part of the long-term light curve of DW UMa obtained by RoboScope (Honeycutt et al. 2003) with the epochs of our observations marked with the vertical bars and the mean out-of-eclipse magnitudes shown with open squares. Our observations in 2000 have been obtained on the rising branch of a deep low state. For clarity, the RoboScope data obtained during eclipse have been removed.
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$\begin{figure} \par\includegraphics*[width=8.8cm]{ms0145f3.eps} \end{figure}$	Figure 3: Eclipse depth as a function of the out-of-eclipse magnitude of DW UMa. Filled circles - Rozhen V-band photometric observations; open circles - unfiltered observations.
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$\begin{figure} \par\includegraphics*[width=18cm,clip]{ms0145f4.eps} \end{figure}$	Figure 4: Periododgram analysis of DW UMa in 2002 - left and in 2003 - right. The insets show the mean superhump shape.
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$\begin{figure} \par\includegraphics*[width=8.8cm,clip]{ms0145f5.eps} \end{figure}$	Figure 5: Mean power spectrum of DW UMa in double logarithmic scale.
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