All Figures

$\begin{figure} \par\includegraphics[width=6.5cm]{2800f1a.eps}\hspace*{5mm} \includegraphics[width=6.5cm]{2800f1b.eps} \end{figure}$ Figure 1: Examples of the fits of reference spectra to the observed magnitudes of V838 Mon. Left panel: pre-eruption and eruption phases. Right panel: decline phase. Symbols - observed magnitudes. Full curves - supergiant spectra. Dotted curves - blackbody distributions. All reference spectra have been reddened with E_B-V = 0.9. The curves are labelled with the epoch of observations (days since 1 Jan. 2002). Note that the curves and the data corresponding to days 40.8, 47.6 and 72.8 ( left panel) have been shifted by -2, -4 and -6 mag, respectively, while those corresponding to days 301, 503, 861 and 1075 (right panel) have been shifted by 2, 5, 8 and 10 mag, respectively. Parameters of the fits can be found in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm]{2800f2a.eps}\vspace*{3mm} \inc... ...2b.eps}\vspace*{3mm} % \includegraphics[width=7.1cm]{2800f2c.eps} % \end{figure}$ Figure 2: Evolution of the effective temperature ( upper), luminosity ( middle) and radius ( bottom) of V838 Mon. The luminosity and radius are in solar units. The abscissa gives the logarithm of time in days counted since 1 Jan. 2002. See text for explanation of the symbols and curves (in the middle and bottom panels).
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In the text

$\begin{figure} \par\resizebox{8.1cm}{!}{\includegraphics[clip]{2800f3.eps}} \end{figure}$ Figure 3: Mass loss rate derived assuming an optically thick wind model (see text for more details) - large symbols. Small symbols - effective radius (the same as in Fig. 2 but plotted as 3 log $~(R/R_{\odot}) - 10.5$ ).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm]{2800f4a.eps}\hspace*{5mm} \includegraphics[width=6.5cm]{2800f4b.eps} \end{figure}$ Figure 4: Infrared excess in pre-eruption and eruption ( left panel) as well as in decline ( right panel). Symbols - observed magnitudes. Full curves - fitted spectra. Dotted and dashed curves ( right panel) - stellar and dust spectral components, respectively. The curves are labelled with the epoch of observations (days since 1 Jan. 2002). A downward arrow for day 258 shows the upper observational limit at 18 $\mu$ m. Note that the curve and the data on day 15.0 ( left panel) have been shifted by 2 mag, while those corresponding to days 395 and 650 ( right pannel) have been shifted by 4 and 8 mag, respectively. The data sources and the parameters of the fitted spectra can be found in Table 2.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm]{2800f2a.eps}\vspace{3mm} \inc... ...2b.eps}\vspace{3mm} % \includegraphics[width=7.1cm]{2800f2c.eps} % \end{figure}$	Figure 2: Evolution of the effective temperature ( upper), luminosity ( middle) and radius ( bottom) of V838 Mon. The luminosity and radius are in solar units. The abscissa gives the logarithm of time in days counted since 1 Jan. 2002. See text for explanation of the symbols and curves (in the middle and bottom panels).
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$\begin{figure} \par\resizebox{8.1cm}{!}{\includegraphics[clip]{2800f3.eps}} \end{figure}$	Figure 3: Mass loss rate derived assuming an optically thick wind model (see text for more details) - large symbols. Small symbols - effective radius (the same as in Fig. 2 but plotted as 3 log $~(R/R_{\odot}) - 10.5$ ).
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