![\begin{figure}
\par\includegraphics[width=8.8cm,clip]{2587fig1.eps}
\end{figure}](/articles/aa/full/2005/33/aa2587-04/Timg15.gif) |
Figure 1:
Observational results for V1974 Cyg compared to our envelope models.
Upper panel: spectral parameters (photospheric radius,
,
and effective temperature,
)
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 .
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. |