All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{2026fig1.eps} \end{figure}$ Figure 1: $10\hbox {$^\prime $ }\times 10\hbox {$^\prime $ }$ finding chart of HS 2219+1824 obtained from the Digitized Sky Survey 2. The coordinates of the CV are $\alpha (2000)=22^{\rm h}21^{\rm m}44.8^{\rm s}$ , $\delta (2000)=+18\hbox {$^\circ $ }40\hbox {$^\prime $ }08.3\hbox {$^{\prime \prime }$ }$ . The star "C'' has been used as comparison for all the differential photometric data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2026fig2.ps} \end{figure}$ Figure 2: Superoutburst of HS 2219+1824 recorded at the OGS telescope. Superhumps set in $\sim$ 1 d after the outburst maximum. The filterless magnitudes are approximatively equivalent to V-band data. Shown as open triangles are the V magnitudes of HS 2219+1824 from the ASAS-3 archive.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{2026fig3.ps} \end{figure}$ Figure 3: Sample light curves of HS 2219+1824 obtained during thesuperoutburst ( top panel) and in quiescence ( bottom panel).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17.6cm,clip]{2026fig4.ps} \end{figure}$ Figure 4: Left and middle panels: AOV periodograms of the entire quiescent data (Kryoneri and IAC80). Right panel: AOV periodogram of the superoutburst data (OGS, 2003 July 11, 14 and 16).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2026fig5.ps} \end{figure}$ Figure 5: Top panel: superoutburst photometry obtained on 2003 July 11, 14 and 16 folded over the superhump period of $\mbox{$P_{\rm sh}$ }=89.05$ min and averaged into 40 phase bins. Bottom panel: quiescent photometry (Kryoneri 2002 and IAC80 2003) folded over the orbital period of 86.2 min and averaged into 40 phase bins. In both cases, the mean magnitude of each individual night was subtracted before folding and binning. The orbital cycle has been duplicated for continuity.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2026fig6.ps} \end{figure}$ Figure 6: Discovery spectrum of HS 2219+1824, obtained with the 2.2 m Telescope at Calar Alto.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2026fig7.ps} \end{figure}$ Figure 7: Left panel: evolution of the ${\rm H\alpha }$ profile during the WHT/ISIS observations. The time co-ordinate runs from UT 19:35 to UT 22:58 (see Table 1). Right panel: selected ${\rm H\alpha }$ profile displaying three peaks.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2026fig8.ps} \end{figure}$ Figure 8: Three-component model of the optical spectrum of HS 2219+1824. The observed spectrum is the topmost grey line. The grey lines below are a white dwarf model spectrum for $\mbox{$T_{{\rm eff}}$ }=16~000$ K, $\log g=8.0$ , and d=215 pc (broad absorption lines), the emission from an isothermal/isobaric slab with $\mbox{$T_{{\rm disc}}$ }=6000$ K and $\Sigma=5.7\times10^{-2}~{\rm g~cm^{-2}}$ , scaled to the observed ${\rm H\alpha }$ flux (emission lines). The secondary star is represented by a M 6 template, assuming $R_{L_2}=9.5\times 10^9$ cm and d=215 pc. The sum of the three components is plotted as black line.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{2026fig9.ps} \end{figure}$ Figure 9: Top: ${\rm H\alpha }$ radial velocity curves of HS 2219+1824 in quiescence computed from the line wings ( filled circles) and the narrow component ( open triangles). Bottom: Scargle periodogram of the ${\rm H\alpha }$ wing velocities.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2026fg10.ps} \end{figure}$ Figure 10: ${\rm H\alpha }$ radial velocity curves of the line wings and the chromospheric emission from the companion. The velocities are folded on the orbital period using T₀=2 452 932.3485(HJD) and no phase binning has been applied. The orbital cycle has been plotted twice for continuity.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2026fg11.ps} \end{figure}$ Figure 11: ${\rm H\alpha }$ , ${\rm H\beta }$ and ${\rm H\gamma }$ trailed spectra diagrams. The spectra have been folded on the orbital period and averaged into 20 phase bins. Notice the narrow ${\rm H\alpha }$ emission component from the secondary star. Another emission component with maximum blue velocity at $\varphi \sim 0.6{-}0.7$ is evident in ${\rm H\beta }$ . Dark represents emission and a full cycle has been repeated for continuity.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.3cm,clip]{2026fg12.ps} \end{figure}$ Figure 12: ${\rm H\alpha }$ , ${\rm H\beta }$ and ${\rm H\gamma }$ Doppler tomograms. Dark represents emission. Notice the ${\rm H\alpha }$ emission at the location of the secondary and the two emission spots in ${\rm H\beta }$ and ${\rm H\gamma }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2026fig1.eps} \end{figure}$	Figure 1: $10\hbox {$^\prime $ }\times 10\hbox {$^\prime $ }$ finding chart of HS 2219+1824 obtained from the Digitized Sky Survey 2. The coordinates of the CV are $\alpha (2000)=22^{\rm h}21^{\rm m}44.8^{\rm s}$ , $\delta (2000)=+18\hbox {$^\circ $ }40\hbox {$^\prime $ }08.3\hbox {$^{\prime \prime }$ }$ . The star "C'' has been used as comparison for all the differential photometric data.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{2026fig2.ps} \end{figure}$	Figure 2: Superoutburst of HS 2219+1824 recorded at the OGS telescope. Superhumps set in $\sim$ 1 d after the outburst maximum. The filterless magnitudes are approximatively equivalent to V-band data. Shown as open triangles are the V magnitudes of HS 2219+1824 from the ASAS-3 archive.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{2026fig3.ps} \end{figure}$	Figure 3: Sample light curves of HS 2219+1824 obtained during thesuperoutburst ( top panel) and in quiescence ( bottom panel).
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$\begin{figure} \par\includegraphics[angle=-90,width=17.6cm,clip]{2026fig4.ps} \end{figure}$	Figure 4: Left and middle panels: AOV periodograms of the entire quiescent data (Kryoneri and IAC80). Right panel: AOV periodogram of the superoutburst data (OGS, 2003 July 11, 14 and 16).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{2026fig6.ps} \end{figure}$	Figure 6: Discovery spectrum of HS 2219+1824, obtained with the 2.2 m Telescope at Calar Alto.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2026fig7.ps} \end{figure}$	Figure 7: Left panel: evolution of the ${\rm H\alpha }$ profile during the WHT/ISIS observations. The time co-ordinate runs from UT 19:35 to UT 22:58 (see Table 1). Right panel: selected ${\rm H\alpha }$ profile displaying three peaks.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{2026fig9.ps} \end{figure}$	Figure 9: Top: ${\rm H\alpha }$ radial velocity curves of HS 2219+1824 in quiescence computed from the line wings ( filled circles) and the narrow component ( open triangles). Bottom: Scargle periodogram of the ${\rm H\alpha }$ wing velocities.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2026fg10.ps} \end{figure}$	Figure 10: ${\rm H\alpha }$ radial velocity curves of the line wings and the chromospheric emission from the companion. The velocities are folded on the orbital period using T₀=2 452 932.3485(HJD) and no phase binning has been applied. The orbital cycle has been plotted twice for continuity.
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$\begin{figure} \par\includegraphics[angle=-90,width=12.3cm,clip]{2026fg12.ps} \end{figure}$	Figure 12: ${\rm H\alpha }$ , ${\rm H\beta }$ and ${\rm H\gamma }$ Doppler tomograms. Dark represents emission. Notice the ${\rm H\alpha }$ emission at the location of the secondary and the two emission spots in ${\rm H\beta }$ and ${\rm H\gamma }$ .
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