All Figures

$\begin{figure} \par\includegraphics[width=6cm,clip]{4935f_1a.ps}\includegraphics[width=6cm,clip]{4935f_1b.ps} \end{figure}$ Figure 1: Geometry of the wind model we used to calculate the line profile of H $\alpha$ and its luminosity. The wind is produced by the central star (small circle at the mid of panels). A fraction of the wind is blocked by an optically thick disk/torus at the center that cut out a cone from the sphere with the opening angle $\pi - 2\theta _0$ . By this way we simulate bipolar geometry of the stellar wind. The shadow belt on the side view ( left) and/or the annulus from the frontal view ( right) represents a part of the shell with the same radial velocity, $-v(r)\cos~(\theta)$ . Radiation from the annulus, cut out by 4 $\tilde\theta$ radians, is blocked by the central disk (the darker part). The angle $\tilde\theta$ is counted in the plane containing the annulus.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{4935f_2.eps} \end{figure}$ Figure 2: Luminosity of H $\alpha$ wings for $\vert\Delta v\vert \ge 200$ km s^-1, $L_{\alpha }$ (200), as a function of the mass-loss rate calculated according to Eq. (12) for parameters $R_{\rm w}$ , $\beta$ and $v_{\infty }$ in Table 1. The observed quantities of $L_{\alpha }$ (200) are denoted by filled diamonds (Table 1).
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In the text

$\begin{figure} \par {\hspace*{6.6cm}\sf Q U I E S C E N T ~ P H A S E S}\\ [-1mm... ...ngle=-90]{4935f_3k.eps} \includegraphics[angle=-90]{4935f_3l.eps}} \end{figure}$ Figure 3: Comparison of the modeled (M) and observed (O) H $\alpha$ line profiles for selected symbiotic stars during their quiescent phases ( top two raws of panels) and active phases ( the bottom raw of panels). The systemic velocity was subtracted. The model is described in Sect. 2.4 and the corresponding parameters are in Table 1. It fits the observed profiles for $\vert\Delta v\vert \protect\ga$ 200 km s^-1. Fluxes are in 10^-11 $\rm ~erg~cm^{-2}~s^{-1}~\AA^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4935f_4.eps} \end{figure}$ Figure 4: Total H $\alpha$ line and wing luminosities, $L_{\alpha }$ (0) and $L_{\alpha }$ (200), respectively, as a function of the observed emission measure $EM_{\rm obs}$ . The total line luminosities are divided by a factor of 5 for a better visual display. Corresponding quantities are from Table 2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{4935f_5.eps} \end{figure}$ Figure 5: Radio observations of Z And at cm wavelengths during quiescence and the recent activity. Steeper continuum spectrum during activity suggests optically thicker conditions than during quiescence. The data are from Brocksopp et al. (2004).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{4935f_2.eps} \end{figure}$	Figure 2: Luminosity of H $\alpha$ wings for $\vert\Delta v\vert \ge 200$ km s^-1, $L_{\alpha }$ (200), as a function of the mass-loss rate calculated according to Eq. (12) for parameters $R_{\rm w}$ , $\beta$ and $v_{\infty }$ in Table 1. The observed quantities of $L_{\alpha }$ (200) are denoted by filled diamonds (Table 1).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4935f_4.eps} \end{figure}$	Figure 4: Total H $\alpha$ line and wing luminosities, $L_{\alpha }$ (0) and $L_{\alpha }$ (200), respectively, as a function of the observed emission measure $EM_{\rm obs}$ . The total line luminosities are divided by a factor of 5 for a better visual display. Corresponding quantities are from Table 2.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{4935f_5.eps} \end{figure}$	Figure 5: Radio observations of Z And at cm wavelengths during quiescence and the recent activity. Steeper continuum spectrum during activity suggests optically thicker conditions than during quiescence. The data are from Brocksopp et al. (2004).
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