All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig1.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{0013fig2.eps} \end{figure}$ Figure 1: Extinction corrected optical spectrum of Hen 2-90, observed with the B&C spectrograph.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig3.eps} \end{figure}$ Figure 2: The [O III] and [S III] lines taken from the Hen 2-90 high-resolution (FEROS) spectrum. They are only two examples of the presence of double-peaked emission line profiles. The velocities obtained from the wings of these lines are given in Table 1. Due to the strong lines, the high velocity wings are not resolved in this figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig4.eps} \end{figure}$ Figure 3: The H I Balmer lines taken from the Hen 2-90 high-resolution (FEROS) spectrum. These lines show an evolution from single-peaked profiles over profiles with a shoulder to double-peaked profiles with decreasing quantum number.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig5.eps} \end{figure}$ Figure 4: Wings of the Balmer lines taken from the Hen 2-90 high-resolution (FEROS) spectrum. They show an increase in velocity from H8 to H $\alpha$ (see Table 1). The wings of H $\alpha$ extend to velocities around 1800 km s^-1; superimposed are the [N II] lines ( $\lambda$ $\lambda$ 6548,6583), as well as the only carbon line identified (C II, $\lambda$ 6578).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig6.eps} \end{figure}$ Figure 5: [S II] line profiles present in the high-resolution spectrum (FEROS) of Hen 2-90. The derived wing velocities are given in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig7.eps} \end{figure}$ Figure 6: The [N II] $\lambda$ 5754 and the [O I] $\lambda$ 6300 lines present in the Hen 2-90 high-resolution (FEROS) spectrum. Notice the presence of a "shoulder'' or almost a second peak. The velocities obtained from the wings of these lines are given in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig8.eps} \end{figure}$ Figure 7: Top panel: HST image of Hen 2-90 replotted with kind permission from Sahai et al. (2002). Overplotted is a big circle that indicates the width of the slit (which is 2 $\hbox {$^{\prime \prime }$ }$ , corresponding to 0.019 pc at a distance of 2 kpc) of our Cassegrain observations from which the line luminosities have been derived. Bottom panel: Sketch of the threefold wind derived from the HST image and used in our calculations. Plotted are the outflowing disk, the polar wind, and the intermediate wind. Indicated are also the opening angles of the polar and disk wind used for the model calculations, and the velocities within the different wind regions as derived from Table 1 and discussed in the text. The whole structure is still embedded in an H II region that extends up to 3 $.\!\!^{\prime\prime}$ 2 corresponding to 0.031 pc, which is 1.6 times larger than the non-spherical wind structure. The bipolar jet and the knots are not taken into account in the non-spherical wind model.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig9.eps} \end{figure}$ Figure 8: Temperature distribution in the wind according to Eq. (5). The starting values T₀ and terminal values $T_{\infty }$ appropriate for the polar/intermediate wind and for the outflowing disk are indicated. The temperature drops quickly (within 100 R_*) to its terminal value, which is found to be about 10 000 K in the polar and the intermediate wind and about 6000 K in the disk wind (see Table 2).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fi10.eps} \end{figure}$ Figure 9: Model results for the [S III] line arising in the outer parts of the intermediate wind. Shown is the increase in line luminosity with distance from the star. The arrow on the right side of the panel indicates the observed value.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fi11.eps} \end{figure}$ Figure 10: Model results for the different [O III] lines listed in the bottom panel. Shown are individual contributions from the polar and intermediate wind and their increase in line luminosity with distance from the star. The bottom panel shows the sum of both contributions, and the arrows on the right side indicate the observed value for each emission line (same line style).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fi12.eps} \end{figure}$ Figure 11: Model results for the [O II] lines. These lines come from the intermediate wind only and from distances where O III has already recombined (see mid-panel of Fig. 10). The arrows on the right side indicate the observed value for each emission line (same line style).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fi13.eps} \end{figure}$ Figure 12: Model results for the [O I] lines. These lines come from the disk wind only. The arrows on the right side indicate the observed value for each emission line (same line style).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig1.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{0013fig2.eps} \end{figure}$	Figure 1: Extinction corrected optical spectrum of Hen 2-90, observed with the B&C spectrograph.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig3.eps} \end{figure}$	Figure 2: The [O III] and [S III] lines taken from the Hen 2-90 high-resolution (FEROS) spectrum. They are only two examples of the presence of double-peaked emission line profiles. The velocities obtained from the wings of these lines are given in Table 1. Due to the strong lines, the high velocity wings are not resolved in this figure.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig4.eps} \end{figure}$	Figure 3: The H I Balmer lines taken from the Hen 2-90 high-resolution (FEROS) spectrum. These lines show an evolution from single-peaked profiles over profiles with a shoulder to double-peaked profiles with decreasing quantum number.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig5.eps} \end{figure}$	Figure 4: Wings of the Balmer lines taken from the Hen 2-90 high-resolution (FEROS) spectrum. They show an increase in velocity from H8 to H $\alpha$ (see Table 1). The wings of H $\alpha$ extend to velocities around 1800 km s^-1; superimposed are the [N II] lines ( $\lambda$ $\lambda$ 6548,6583), as well as the only carbon line identified (C II, $\lambda$ 6578).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig6.eps} \end{figure}$	Figure 5: [S II] line profiles present in the high-resolution spectrum (FEROS) of Hen 2-90. The derived wing velocities are given in Table 1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fig7.eps} \end{figure}$	Figure 6: The [N II] $\lambda$ 5754 and the [O I] $\lambda$ 6300 lines present in the Hen 2-90 high-resolution (FEROS) spectrum. Notice the presence of a "shoulder'' or almost a second peak. The velocities obtained from the wings of these lines are given in Table 1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fi10.eps} \end{figure}$	Figure 9: Model results for the [S III] line arising in the outer parts of the intermediate wind. Shown is the increase in line luminosity with distance from the star. The arrow on the right side of the panel indicates the observed value.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fi11.eps} \end{figure}$	Figure 10: Model results for the different [O III] lines listed in the bottom panel. Shown are individual contributions from the polar and intermediate wind and their increase in line luminosity with distance from the star. The bottom panel shows the sum of both contributions, and the arrows on the right side indicate the observed value for each emission line (same line style).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fi12.eps} \end{figure}$	Figure 11: Model results for the [O II] lines. These lines come from the intermediate wind only and from distances where O III has already recombined (see mid-panel of Fig. 10). The arrows on the right side indicate the observed value for each emission line (same line style).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0013fi13.eps} \end{figure}$	Figure 12: Model results for the [O I] lines. These lines come from the disk wind only. The arrows on the right side indicate the observed value for each emission line (same line style).
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