All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4690F001.eps}\end{figure}$ Figure 1: Isovelocity intensity maps computed with the SIMECA code, seen with an inclination angle of 45 $\hbox {$^\circ $ }$ , and showing the effect of the disk kinematics (mainly Keplerian rotation) as a function of wavelength, 21 636, 21 641, 21 646, 21 651, 21 656, 21 661, 21 666, 21 671, and 21 676 $\AA$ across the Br $\gamma$ line within a spectral bandwidth of 5 $\AA$ .
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In the text

$\begin{figure} \par\begin{tabular}{ccccccc} \includegraphics[width=1.9cm,height=... ...udegraphics[width=1.9cm,height=1.9cm]{4690F022.eps}\\ \end{tabular}\end{figure}$ Figure 2: Intensity maps computed with the SIMECA code showing the formation of a ring ranging from 0 to 60 stellar radii by 10 R_* steps. Seen pole-on ( upper row), at 45 $\hbox {$^\circ $ }$ ( center), and equator-on ( lower row).
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In the text

$\begin{figure} \par\includegraphics[width=4.4cm,height=4.5cm,clip]{4690F023.eps}... ...m} \includegraphics[width=4.3cm,height=4.5cm,clip]{4690F028.eps}\\ \end{figure}$ Figure 3: Br $\gamma$ line profiles ( upper line) and visibilities as a function of baseline ( lower line) for different ring sizes: r=0 (plain line), r=10 (dotted line), r=20 (dashed line), r=30 (dash-dotted line), r=40 (dash-dot-dot-dot line), r=50 (long-dash line), and for r= 60, 70, and 80 R_* (plain line) corresponding to the maps given in Fig. 2. These curves are plotted for 3 inclination angles, i.e. Pole-on ( left), 45 $\hbox {$^\circ $ }$ ( center), equator-on ( right), and for a baseline position along the equatorial disk.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,height=6.1cm,clip]{4690F028.eps}... ...4mm} \includegraphics[width=5.8cm,height=6.1cm,clip]{4690F029.eps} \end{figure}$ Figure 4: Visibilities for the ring model as a function of the baseline length for a baseline orientation along ( left) and perpendicular ( right) to the equatorial disk as a function of the disk dissipation.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4690F030.eps}\end{figure}$ Figure 5: Spectral energy distribution (SED) as a function of the ring size, for the lower plain line: central star only, r=0 (dotted line), r=10 (dashed line), r=20 (dash-dotted line), r=30 (dash-dot-dot-dot line), r=40 (long-dash line), and for r= 50, 60 70 and 80 (plain line). Since the disk is nearly optically thin the SED is nearly independent of the inclination angle between the star rotation axis and the observer line of sight.
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In the text

$\begin{figure} \par\begin{tabular}{ccccc} \includegraphics[width=3.2cm,height=3.... ...udegraphics[width=3.2cm,height=3.2cm]{4690F042.eps}\\ \end{tabular}\end{figure}$ Figure 6: Intensity maps computed with the SIMECA code showing the vanishing of the circumstellar disk by decreasing the mass flux and thus the global mass loss rates: $4.7\times 10^{-10}$ , $2.3\times 10^{-10}$ , $9.4\times 10^{-11}$ , $4.7\times 10^{-11}$ , $2.3\times 10^{-11}~M_{\odot}$ year^-1 from the left to the right, as seen pole-on ( upper row), at 45 $\hbox {$^\circ $ }$ ( center), and equator-on ( lower row).
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In the text

$\begin{figure} \par\includegraphics[width=4.6cm,height=4.7cm,clip]{4690F043.eps}... ...*{5mm} \includegraphics[width=4.5cm,height=4.7cm,clip]{4690F048.eps}\end{figure}$ Figure 7: Br $\gamma$ line profiles ( upper row) and visibilities as a function of baseline ( lower row) for different mass loss rates, $4.7\times 10^{-10}$ (plain-line), $2.3\times 10^{-10}$ (dotted-line), $9.4\times 10^{-11}$ (dashed-line), and $4.7 \times10^{-11}~ M _{\odot }~$ year^-1 corresponding to the maps given in Fig. 6. These curves are plotted for 3 inclination angles, i.e. Pole-on ( left), 45 $\hbox {$^\circ $ }$ ( center), equator-on ( right) and for a baseline position along the equatorial disk.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4690F049.eps} \end{figure}$ Figure 8: Spectral energy distribution (SED) as a function of the mass loss rate: only the central star (lower plain line), $4.7\times 10^{-10}$ (dotted-line), $2.3\times 10^{-10}$ (dashed-line), $9.4\times 10^{-11}$ (dash-dot-line) and $4.7\times 10^{-11}$ (dash-dot-dot line) $M _{\odot }$ year^-1. Since the disk is nearly optically thin, the SED is nearly independent of the inclination angle between the star rotation axis and the observer's line of sight.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,height=6.1cm,clip]{4690F024.eps}... ...{4mm} \includegraphics[width=5.8cm,height=6.1cm,clip]{4690F044.eps} \end{figure}$ Figure 9: Br $\gamma$ line profiles from the ring ( left) and mass flux scenarios computed for an inclination angle of 45 $\hbox {$^\circ $ }$ between the star rotation axis and the observer's line of sight as a function of the disk dissipation.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,height=6.2cm,clip]{4690F028.eps}... ...*{4mm} \includegraphics[width=5.8cm,height=6.2cm,clip]{4690F048.eps}\end{figure}$ Figure 10: Visibilities as a function of the baseline length for a baseline orientation along the equatorial disk as a function of the disk dissipation: following the ring model ( left) and the decreasing mass flux scenario ( right).
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In the text

$\begin{figure} \par\includegraphics[width=7.07cm,height=6.47cm,clip]{4690F050.eps}\end{figure}$ Figure 11: GG Tauri real part of the 1.4 mm continuum visibility as a function of the IRAM baseline length (dots with error bars) with a model (plain line) where 90% of the flux comes from a ring and the rest from an extended disk from Fig. 2 in Guilloteau et al. (1999). Note that this is the real part of the visibility (which can be negative!) whereas in our simulation we plotted the visibility modulus that is always between 0 and 1. The global shape of the visibility curve is the same as for our ring model from Fig. 3 seen pole-on.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4690F001.eps}\end{figure}$	Figure 1: Isovelocity intensity maps computed with the SIMECA code, seen with an inclination angle of 45 $\hbox {$^\circ $ }$ , and showing the effect of the disk kinematics (mainly Keplerian rotation) as a function of wavelength, 21 636, 21 641, 21 646, 21 651, 21 656, 21 661, 21 666, 21 671, and 21 676 $\AA$ across the Br $\gamma$ line within a spectral bandwidth of 5 $\AA$ .
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$\begin{figure} \par\begin{tabular}{ccccccc} \includegraphics[width=1.9cm,height=... ...udegraphics[width=1.9cm,height=1.9cm]{4690F022.eps}\\ \end{tabular}\end{figure}$	Figure 2: Intensity maps computed with the SIMECA code showing the formation of a ring ranging from 0 to 60 stellar radii by 10 R_* steps. Seen pole-on ( upper row), at 45 $\hbox {$^\circ $ }$ ( center), and equator-on ( lower row).
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$\begin{figure} \par\includegraphics[width=5.8cm,height=6.1cm,clip]{4690F028.eps}... ...4mm} \includegraphics[width=5.8cm,height=6.1cm,clip]{4690F029.eps} \end{figure}$	Figure 4: Visibilities for the ring model as a function of the baseline length for a baseline orientation along ( left) and perpendicular ( right) to the equatorial disk as a function of the disk dissipation.
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$\begin{figure} \par\includegraphics[width=5.8cm,height=6.1cm,clip]{4690F024.eps}... ...{4mm} \includegraphics[width=5.8cm,height=6.1cm,clip]{4690F044.eps} \end{figure}$	Figure 9: Br $\gamma$ line profiles from the ring ( left) and mass flux scenarios computed for an inclination angle of 45 $\hbox {$^\circ $ }$ between the star rotation axis and the observer's line of sight as a function of the disk dissipation.
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$\begin{figure} \par\includegraphics[width=5.8cm,height=6.2cm,clip]{4690F028.eps}... ...*{4mm} \includegraphics[width=5.8cm,height=6.2cm,clip]{4690F048.eps}\end{figure}$	Figure 10: Visibilities as a function of the baseline length for a baseline orientation along the equatorial disk as a function of the disk dissipation: following the ring model ( left) and the decreasing mass flux scenario ( right).
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