Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-0,width=17cm,height=23.0cm,bbllx=40pt,bblly=47pt,bburx=527pt,bbury=713pt,clip=]{h4010f1.ps} \end{figure}$ Figure 1: Line intensity profiles of H $\alpha$ as a function of heliocentric radial velocity. All lines were normalized to the peak flux. A few stars were observed more than once. Profile variability was found in MWC 342, MWC 939, MWC 1055, HD 87643, and Hen 485 (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=-0,width=17.0cm,height=22.4cm,bbllx=34pt,bblly=47pt,bburx=550pt,bbury=740pt,clip=]{h4010f2a.ps} \end{figure}$ Figure 2: a) Line intensity profiles of the forbidden lines as a function of heliocentric radial velocity. All lines were normalized to the peak flux. From bottom to top the profiles of [O I] $\lambda$ 6300 Å, [Fe II] $\lambda$ 7155 Å, [N II] $\lambda$ 6583 Å, and [S III] $\lambda$ 6312 Å are plotted with shifts in relative intensity of 0, 0.75, 1.5, and 2.25, respectively.
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In the text

$\begin{figure} \par\addtocounter{figure}{-1} \includegraphics[angle=-0,width=17.0cm,bbllx=34pt,bblly=390pt,bburx=550pt,bbury=745pt,clip=]{h4010f2b.ps}\end{figure}$ Figure 2: b) continued.
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In the text

$\begin{figure} \par\includegraphics[angle=-0,width=17.0cm,bbllx=35pt,bblly=45pt,bburx=534pt,bbury=344pt,clip=]{h4010f3.ps} \end{figure}$ Figure 3: Line intensity profiles of He I $\lambda$ 5876 Å emission line profiles as a function of heliocentric radial velocity. For MWC 137 the line observed in 2002 is shown.
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In the text

$\begin{figure} \par\resizebox{6cm}{!}{\includegraphics[angle=0,bbllx=20pt,bblly=255pt,bburx=370pt,bbury=600pt,clip=]{h4010f4.ps}} \end{figure}$ Figure 4: [O I] $\lambda$ 6300 Å profile of HD 45677. The double peak is just resolved with a peak separation of 6 km s^-1.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90,bbllx=190pt,bblly=55pt,bburx=547pt,bbury=715pt,clip=]{h4010f5.ps}} \end{figure}$ Figure 5: FWHM of [O I] vs. H $\alpha$ . Here and in the following figures the solid line designates a ratio of line widths of 1.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90,width=8.7cm,bbllx=190pt,bblly=55pt,bburx=547pt,bbury=715pt,clip=]{h4010f6.ps}} \par\end{figure}$ Figure 6: FWHM of [O I] vs. He I.
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In the text

$\begin{figure} { \resizebox{0.47\hsize}{!}{\includegraphics[width=8.7cm,angle=-9... ...,bbllx=50pt,bblly=30pt,bburx=555pt,bbury=575pt,clip=]{h4010f7c.ps}} \end{figure}$ Figure 7: FWHM of [Fe II] vs. [O I] (upper left panel), [O I] vs. [N II] (upper right panel), and [Fe II] vs. [N II] (lower panel).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90,bbllx=180pt,bblly=55pt,bburx=570pt,bbury=720pt,clip=]{h4010f8.ps}} \end{figure}$ Figure 8: Line splitting of H $\alpha$ vs. [O I]. The solid line represents the locus of equal splitting for both lines.
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In the text

$\begin{figure} \par\resizebox{0.47\hsize}{!}{\includegraphics[width=8.7cm,angle=... ...bbllx=190pt,bblly=60pt,bburx=565pt,bbury=430pt,clip=]{h4010f9b.ps}} \end{figure}$ Figure 9: Line splitting of [O I] vs. [N II] (left panel) and of [O I] vs. [Fe II] (right panel). Upper limits are plotted as arrows. Equal peak separation is represented by the diagonal lines in each panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,bbllx=50pt,bblly=60pt,bburx=550pt,bbury=770pt,clip=]{h4010f10.ps} \end{figure}$ Figure 10: Profiles of optically thin lines for different inclination angles i and a dust disk in the equatorial plane with various optical depths, $\tau = 1000$ (solid line), $\tau = 1$ (short dashed line), and $\tau = 0.1$ (long dashed line). D₀ and $R_{\rm d}$ were set to 1.0 and 1 ${R}_{\star }$ , respectively. The ordinate is the flux normalized to the maximum. The abscissa is the radial velocity normalized to the maximum wind speed.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bbllx=45pt,bblly=48pt,bburx=375pt,bbury=770pt,clip=]{h4010f11.ps}} \end{figure}$ Figure 11: Line profiles for $D_0 = 5~\times~ 10^2$ (solid line), $3~\times~ 10^4$ (short dashed line), and $1\times 10^6$ (long dashed line). For the dust ring an optical depth of $\tau _{\rm d} = 1$ and an inner radius of $R_{\rm d} = 1000~{R}_{\star}\$ was adopted.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bbllx=45pt,bblly=48pt,bburx=375pt,bbury=770pt,clip=]{h4010f12.ps}} \end{figure}$ Figure 12: Line profiles for $D_0 = 5~\times~ 10^2$ (solid line), $3~\times~ 10^4$ (short dashed line), and $1\times 10^6$ (long dashed line). For the dust ring an optical depth of $\tau _{\rm d} = 1000$ and an inner radius of $R_{\rm d} = 1000~{R}_{\star}\$ was adopted.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bbllx=45pt,bblly=48pt,bburx=375pt,bbury=770pt,clip=]{h4010f13.ps}} \end{figure}$ Figure 13: Line profiles for an equatorial disk and polar cone geometry with $\tau _{\rm d} = 1$ , $D_0 = 3\times 10^5$ and $R_{\rm d} = 500~{R}_{\star}$ . For the equatorial disk (solid line) an opening angle of $30\hbox {$^\circ $ }$ measured from the equatorial plane was adopted. The polar cone (dashed line) is the complementary volume with an opening angle of $60\hbox {$^\circ $ }$ measured from the polar axis.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bbllx=45pt,bblly=48pt,bburx=375pt,bbury=770pt,clip=]{h4010f14.ps}} \end{figure}$ Figure 14: Line profiles for the same geometry as in Fig. 13 but for $\tau _{\rm d} = 1000$ and $D_0 = 1\times 10^6$ . The equatorial disk and polar cone profiles are plotted as solid and dashed lines, respectively.
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In the text

$\begin{figure} \par\resizebox{6cm}{!}{\includegraphics[angle=-90,bbllx=52pt,bblly=62pt,bburx=314pt,bbury=318pt,clip=]{h4010f15.ps}} \end{figure}$ Figure 15: Line profiles for a wind model with $v_{\rm max} = 300$ km s^-1 at the pole, $v_{\rm eq} = 25$ km s^-1 at the equator, i.e. $f(\pi /2) = 0.08$ , inclination $i =45\hbox {$^\circ $ }$ , and macroturbulence velocities of $v_{\rm t} =$ 15, 20, 30, 35 km s^-1, respectively (from bottom to top). D₀ and $R_{\rm d}$ are $3\times 10^5$ and $1000~{R}_{\star}$ , respectively.
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In the text

$\begin{figure} \par\resizebox{6cm}{!}{\includegraphics[angle=0,bbllx=45pt,bblly=505pt,bburx=370pt,bbury=770pt,clip=]{h4010f16.ps}} \end{figure}$ Figure 16: Simultaneous appearance of split and single-peaked lines for a polar cone with an opening angle of $80\hbox {$^\circ $ }$ (dashed line) and an opening angle of $90\hbox {$^\circ $ }$ (solid line) with $R_{\rm d} = 1000~{R}_{\star}\$ , $\tau _{\rm d} = 0.5$ , $D_0 = 3\times 10^5$ (dashed line) and $D_0 = 5\times 10^{3}$ (solid line). The D₀ values correspond to [O I] and [Fe II] for N₀ = 10¹² cm^-3, respectively.
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In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D1a.eps} \end{figure}$ Figure D.1: Sections of the spectra around the lines of [O I] $\lambda$ 6300 Å, [S III] $\lambda$ 6312 Å, and Mg II $\lambda$ 6318 Å.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D1b.eps} \end{figure}$ Figure D.1: [O I] $\lambda$ 6300 Å, continued. HD 87643 was observed twice, in 1986 (solid line) and 1988 (dashed line).

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D1c.eps} \end{figure}$ Figure D.1: [O I] $\lambda$ 6300 Å, continued.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D2a.eps} \end{figure}$ Figure D.2: Sections of the spectra around the line of [N II] $\lambda$ 6583 Å. Several stars also show emission of Fe II $\lambda$ 6587 Å. MWC 84 in addition exhibits C II $\lambda$ 6578 Å.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D2b.eps} \end{figure}$ Figure D.2: [N II] $\lambda$ 6583 Å, continued. The line visible in HD 87643 is Fe II $\lambda$ 6587 Å.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D2c.eps} \end{figure}$ Figure D.2: [N II] $\lambda$ 6583 Å, continued. The line visible in CPD-52 $\hbox {$^\circ $ }$ 9243 is Fe II $\lambda$ 6587 Å.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D3a.eps} \end{figure}$ Figure D.3: Sections of the spectra around the line [Fe II] $\lambda$ 7155 Å. Also visible is [Fe II] $\lambda$ 7172 Å.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D3b.eps} \end{figure}$ Figure D.3: [Fe II] $\lambda$ 7155 Å, continued. For MWC 1055 the telluric absorption lines have not been corrected.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D3c.eps} \end{figure}$ Figure D.3: [Fe II] $\lambda$ 7155 Å, continued.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D4.eps} \end{figure}$ Figure D.4: Sections of the spectra around [Fe II] $\lambda$ 4287 observed for two stars.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D5a.eps} \end{figure}$ Figure D.5: Permitted Fe II line profiles. The figure shows sections of the spectra around the permitted line of Fe II $\lambda$ 6456 Å.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D5b.eps} \end{figure}$ Figure D.5: Fe II $\lambda$ 6456 Å, continued.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D6.eps} \end{figure}$ Figure D.6: Permitted Fe II lines around $\lambda$ 4560 Å observed for three stars.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D7a.eps} \end{figure}$ Figure D.7: Sections of the spectra around the lines of He I $\lambda$ 5876 Å and the Na I D doublet. The upper spectrum of MWC 84 has been overplotted with a stretch factor of 10 in the normalized flux.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D7b.eps} \end{figure}$ Figure D.7: He I $\lambda$ 5876 Å, continued.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D7c.eps} \end{figure}$ Figure D.7: He I $\lambda$ 5876 Å, continued.

In the text

$\begin{figure}\par\includegraphics[width=18cm,clip=]{h4010D8.eps} \end{figure}$ Figure D.8: Sections of the spectra around He I $\lambda$ 6678 Å observed for four stars.

In the text

$\begin{figure} \par\includegraphics[angle=-0,width=17cm,height=23.0cm,bbllx=40pt,bblly=47pt,bburx=527pt,bbury=713pt,clip=]{h4010f1.ps} \end{figure}$	Figure 1: Line intensity profiles of H $\alpha$ as a function of heliocentric radial velocity. All lines were normalized to the peak flux. A few stars were observed more than once. Profile variability was found in MWC 342, MWC 939, MWC 1055, HD 87643, and Hen 485 (see text).
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$\begin{figure} \par\includegraphics[angle=-0,width=17.0cm,height=22.4cm,bbllx=34pt,bblly=47pt,bburx=550pt,bbury=740pt,clip=]{h4010f2a.ps} \end{figure}$	Figure 2: a) Line intensity profiles of the forbidden lines as a function of heliocentric radial velocity. All lines were normalized to the peak flux. From bottom to top the profiles of [O I] $\lambda$ 6300 Å, [Fe II] $\lambda$ 7155 Å, [N II] $\lambda$ 6583 Å, and [S III] $\lambda$ 6312 Å are plotted with shifts in relative intensity of 0, 0.75, 1.5, and 2.25, respectively.
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$\begin{figure} \par\addtocounter{figure}{-1} \includegraphics[angle=-0,width=17.0cm,bbllx=34pt,bblly=390pt,bburx=550pt,bbury=745pt,clip=]{h4010f2b.ps}\end{figure}$	Figure 2: b) continued.
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$\begin{figure} \par\includegraphics[angle=-0,width=17.0cm,bbllx=35pt,bblly=45pt,bburx=534pt,bbury=344pt,clip=]{h4010f3.ps} \end{figure}$	Figure 3: Line intensity profiles of He I $\lambda$ 5876 Å emission line profiles as a function of heliocentric radial velocity. For MWC 137 the line observed in 2002 is shown.
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$\begin{figure} \par\resizebox{6cm}{!}{\includegraphics[angle=0,bbllx=20pt,bblly=255pt,bburx=370pt,bbury=600pt,clip=]{h4010f4.ps}} \end{figure}$	Figure 4: [O I] $\lambda$ 6300 Å profile of HD 45677. The double peak is just resolved with a peak separation of 6 km s^-1.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90,bbllx=190pt,bblly=55pt,bburx=547pt,bbury=715pt,clip=]{h4010f5.ps}} \end{figure}$	Figure 5: FWHM of [O I] vs. H $\alpha$ . Here and in the following figures the solid line designates a ratio of line widths of 1.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90,width=8.7cm,bbllx=190pt,bblly=55pt,bburx=547pt,bbury=715pt,clip=]{h4010f6.ps}} \par\end{figure}$	Figure 6: FWHM of [O I] vs. He I.
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$\begin{figure} { \resizebox{0.47\hsize}{!}{\includegraphics[width=8.7cm,angle=-9... ...,bbllx=50pt,bblly=30pt,bburx=555pt,bbury=575pt,clip=]{h4010f7c.ps}} \end{figure}$	Figure 7: FWHM of [Fe II] vs. [O I] (upper left panel), [O I] vs. [N II] (upper right panel), and [Fe II] vs. [N II] (lower panel).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=-90,bbllx=180pt,bblly=55pt,bburx=570pt,bbury=720pt,clip=]{h4010f8.ps}} \end{figure}$	Figure 8: Line splitting of H $\alpha$ vs. [O I]. The solid line represents the locus of equal splitting for both lines.
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$\begin{figure} \par\resizebox{0.47\hsize}{!}{\includegraphics[width=8.7cm,angle=... ...bbllx=190pt,bblly=60pt,bburx=565pt,bbury=430pt,clip=]{h4010f9b.ps}} \end{figure}$	Figure 9: Line splitting of [O I] vs. [N II] (left panel) and of [O I] vs. [Fe II] (right panel). Upper limits are plotted as arrows. Equal peak separation is represented by the diagonal lines in each panel.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bbllx=45pt,bblly=48pt,bburx=375pt,bbury=770pt,clip=]{h4010f11.ps}} \end{figure}$	Figure 11: Line profiles for $D_0 = 5~\times~ 10^2$ (solid line), $3~\times~ 10^4$ (short dashed line), and $1\times 10^6$ (long dashed line). For the dust ring an optical depth of $\tau _{\rm d} = 1$ and an inner radius of $R_{\rm d} = 1000~{R}_{\star}\$ was adopted.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bbllx=45pt,bblly=48pt,bburx=375pt,bbury=770pt,clip=]{h4010f12.ps}} \end{figure}$	Figure 12: Line profiles for $D_0 = 5~\times~ 10^2$ (solid line), $3~\times~ 10^4$ (short dashed line), and $1\times 10^6$ (long dashed line). For the dust ring an optical depth of $\tau _{\rm d} = 1000$ and an inner radius of $R_{\rm d} = 1000~{R}_{\star}\$ was adopted.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[bbllx=45pt,bblly=48pt,bburx=375pt,bbury=770pt,clip=]{h4010f14.ps}} \end{figure}$	Figure 14: Line profiles for the same geometry as in Fig. 13 but for $\tau _{\rm d} = 1000$ and $D_0 = 1\times 10^6$ . The equatorial disk and polar cone profiles are plotted as solid and dashed lines, respectively.
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$\begin{figure} \par\resizebox{6cm}{!}{\includegraphics[angle=-90,bbllx=52pt,bblly=62pt,bburx=314pt,bbury=318pt,clip=]{h4010f15.ps}} \end{figure}$	Figure 15: Line profiles for a wind model with $v_{\rm max} = 300$ km s^-1 at the pole, $v_{\rm eq} = 25$ km s^-1 at the equator, i.e. $f(\pi /2) = 0.08$ , inclination $i =45\hbox {$^\circ $ }$ , and macroturbulence velocities of $v_{\rm t} =$ 15, 20, 30, 35 km s^-1, respectively (from bottom to top). D₀ and $R_{\rm d}$ are $3\times 10^5$ and $1000~{R}_{\star}$ , respectively.
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