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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2587fig1.eps} \end{figure}$ Figure 1: Observational results for V1974 Cyg compared to our envelope models. Upper panel: spectral parameters (photospheric radius, $R_{\rm photos}$ , and effective temperature, $kT_{\rm eff}$ ) for ROSAT observations on days 255(A), 261(B), 291(C), 434(D) and 511(E) after outburst (from Balman et al. 1998). Solid line contours for a distance of 2.5 kpc; dotted line contours for all the distance range of 1.7-3.3 kpc). Observational results are overplotted on ONe25 (dashed) and ONe50 (solid) envelope models, for white dwarf masses 0.9, 1.0 and 1.1 $M_{\odot }$ . Numbers indicate days between observations. Vertical lines are orientative for comparison with the lower panels. Middle panel: envelope masses for ONe25 models. Numbers indicate days spent by the envelope model between two adjacent points. Lower panel: same as in middle panel for ONe50 models.
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