Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{MS3365f1.eps} \end{figure}$ Figure 1: Relationship between the free parameter m1 and the disk opening angle in degree (180 $\hbox {$^\circ $ }$ corresponds to a spherical circumstellar envelope).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{MS3365f2.eps} \end{figure}$ Figure 2: Relationship between the disk opening angle in degree and the 2.16 $\mu$ m flux (in magnitude).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{MS3365f3.eps} \end{figure}$ Figure 3: Zoom on the relationship between the disk opening angle (from 0 to 40 $\hbox {$^\circ $ }$ ) and the 2.16 $\mu$ m flux (in magnitude).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{MS3365f4.eps} \end{figure}$ Figure 4: Relationship between logarithm of the mass loss of the star and the 2.16 $\mu$ m flux (in magnitude).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{MS3365f5.eps} \end{figure}$ Figure 5: Relationship between logarithm of the mass loss of the star and the logarithm of the Br $\gamma$ continuum emission. This correlation is of the same nature has found by Scuderi et al. (1998) for O-B supergiants.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{MS3365f6.eps} \end{figure}$ Figure 6: Relationship between logarithm of the mass of the circumstellar disk and the 2.16 $\mu$ m flux (in magnitude).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{MS3365f7.eps} \end{figure}$ Figure 7: Relationship between the disk opening angle in degree and the 2.16 $\mu$ m flux (in magnitude) for different densities at the base of the stellar photosphere indicated on the plot (in g cm^-3). We have overplotted the opening angles and the 2.16 $\mu$ m flux determined by Waters et al. (1987).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{MS3365f8.eps} \end{figure}$ Figure 8: Relationship between logarithm of the mass loss of the star and the 2.16 $\mu$ m flux (in magnitude) for different densities at the base of the stellar photosphere indicated on the plot (in g cm^-3).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{MS3365f9.eps} \end{figure}$ Figure 9: Visibility curves for a 25 000 K, 10 $R_\odot$ radius Be star seen at 200 parsecs as a function of baseline (in meters) for different wind densities at the base of the photosphere (in g cm^-3).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{MS3365f10.eps} \end{figure}$ Figure 10: Visibility curves for a 10 $R_\odot$ radius Be star seen at 200 parsecs with a wind densities at the base of the photosphere of 10^-12 g cm^-3, as a function of baseline (in meters) for different effective temperatures, respectively 16 000, 20 000, 25 000, 30 000, 35 000 and 40 000 K. Since the differences are very small, the curves are superimposed.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{MS3365f1.eps} \end{figure}$	Figure 1: Relationship between the free parameter m1 and the disk opening angle in degree (180 $\hbox {$^\circ $ }$ corresponds to a spherical circumstellar envelope).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{MS3365f2.eps} \end{figure}$	Figure 2: Relationship between the disk opening angle in degree and the 2.16 $\mu$ m flux (in magnitude).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{MS3365f3.eps} \end{figure}$	Figure 3: Zoom on the relationship between the disk opening angle (from 0 to 40 $\hbox {$^\circ $ }$ ) and the 2.16 $\mu$ m flux (in magnitude).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{MS3365f4.eps} \end{figure}$	Figure 4: Relationship between logarithm of the mass loss of the star and the 2.16 $\mu$ m flux (in magnitude).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{MS3365f5.eps} \end{figure}$	Figure 5: Relationship between logarithm of the mass loss of the star and the logarithm of the Br $\gamma$ continuum emission. This correlation is of the same nature has found by Scuderi et al. (1998) for O-B supergiants.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{MS3365f6.eps} \end{figure}$	Figure 6: Relationship between logarithm of the mass of the circumstellar disk and the 2.16 $\mu$ m flux (in magnitude).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{MS3365f7.eps} \end{figure}$	Figure 7: Relationship between the disk opening angle in degree and the 2.16 $\mu$ m flux (in magnitude) for different densities at the base of the stellar photosphere indicated on the plot (in g cm^-3). We have overplotted the opening angles and the 2.16 $\mu$ m flux determined by Waters et al. (1987).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{MS3365f8.eps} \end{figure}$	Figure 8: Relationship between logarithm of the mass loss of the star and the 2.16 $\mu$ m flux (in magnitude) for different densities at the base of the stellar photosphere indicated on the plot (in g cm^-3).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{MS3365f9.eps} \end{figure}$	Figure 9: Visibility curves for a 25 000 K, 10 $R_\odot$ radius Be star seen at 200 parsecs as a function of baseline (in meters) for different wind densities at the base of the photosphere (in g cm^-3).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{MS3365f10.eps} \end{figure}$	Figure 10: Visibility curves for a 10 $R_\odot$ radius Be star seen at 200 parsecs with a wind densities at the base of the photosphere of 10^-12 g cm^-3, as a function of baseline (in meters) for different effective temperatures, respectively 16 000, 20 000, 25 000, 30 000, 35 000 and 40 000 K. Since the differences are very small, the curves are superimposed.
Open with DEXTER