All Figures

$\begin{figure} \par\includegraphics[width=8.65cm,clip]{5775fig1} \end{figure}$ Figure 1: Schematic representation of the free-standing vertical prominence slab. The slab has a geometrical extension L along the line-of-sight to the observer, at the altitude H above the limb. The prominence plasma is moving radially outwards at the velocity $\vec{V}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5775fig2} \end{figure}$ Figure 2: Angle-averaged incident profiles in the prominence frame in the He I 584 line for a prominence located at 50 000 km above the limb, and for velocities ranging from 0 (solid line) to 240 km s^-1 (step = 80 km s^-1). The incident profile is shifted towards the red when the velocity increases.
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In the text

$\begin{figure} \par\includegraphics[width=14.1cm,clip]{5775fig3} \end{figure}$ Figure 3: Differences between CRD (dashed line) and PRD (solid line) for the profiles of the three helium lines at different velocities: 0, 80, 160, and 240 km s^-1 from top to bottom. Abscissa is $\Delta \lambda$ (distance to line centre) in Å and vertical axis is specific intensity in erg s^-1 cm^-2 sr^-1 Å^-1. Model parameters are altitude H=50 000 km, width L=650 km, temperature T=6500 K, and pressure p=0.1 dyn cm^-2.
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In the text

$\begin{figure} \par\includegraphics[width=14.2cm,clip]{5775fig4} \end{figure}$ Figure 4: Same as Fig. 3, with the abscissa now in Doppler units and limited to 10 Doppler widths around line centre, and the intensities on the vertical axis now shown on a log scale. The thin solid line shows the incident line profile, gradually shifting towards the red as the prominence is moving radially upwards.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5775fig5} \end{figure}$ Figure 5: Comparison of the relative contribution of the Doppler core in the emitted line integrated intensities between CRD (dotted line) and PRD (solid line) calculations for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å( $\Diamond$ ). Same model as for Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5775fig6} \end{figure}$ Figure 6: Comparison of the relative integrated intensities (integrated intensities normalised to the intensity at rest) between CRD (dotted line) and PRD (solid line) calculations for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å ( $\Diamond$ ). Same model as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5775fig7} \end{figure}$ Figure 7: Emergent intensities in erg s^-1 cm^-2 sr^-1 as a function of radial velocity for He I $\lambda \lambda$ 584 ( upper left panel) and 537 Å ( upper right) and He II $\lambda$ 304 Å ( lower left). The lower right panel shows the variation of the relative populations (populations normalised to the population at zero velocity) with speed for levels ¹S 1s2p of He I (5: upper level of the resonance transition at 584 Å) and n=2 of He II (31: first excited state of He II, i.e. upper level of the resonance transition at 304 Å). Dotted lines are for CRD computations and solid lines for PRD computations. Same model as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5775fig8} \end{figure}$ Figure 8: Relative intensity as a function of velocity at 8000 K (solid line) and 15 000 K (dotted line) for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å ( $\Diamond$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{5775fg10} \end{figure}$ Figure 10: Relative intensity as a function of velocity at 0.01 dyn cm^-2 (dotted line) and 0.1 dyn cm^-2 (solid line) for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å ( $\Diamond$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5775fg12} \end{figure}$ Figure 12: Population density of the ground level of He II as a function of velocity. The thickest lines refer to the mean population, the medium-thick line shows the level population at the surface of the slab, and the thinnest line corresponds to the population at slab centre. Solid lines: reference model with P=0.1 dyn cm^-2; dashed lines: low-pressure model with P=0.01 dyn cm^-2.
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{5775fg13} \end{figure}$ Figure 13: Relative intensity as a function of velocity for a slab width of 200 km (dotted line) and 2000 km (solid line) for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å ( $\Diamond$ ).
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In the text

$\begin{figure} \par\includegraphics[width=14.1cm,clip]{5775fig9} \end{figure}$ Figure 9: Line profiles for T=8000 K (solid line) and T=15 000 K (dashed line), with p=0.1 dyn cm^-2, and L=2000 km, at different velocities: 0, 40, 80, 120, 200 and 400 km s^-1 from top to bottom. Abscissa is $\Delta \lambda$ in Å and vertical axis is specific intensity in erg s^-1 cm^-2 sr^-1 Å^-1.
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In the text

$\begin{figure} \par\includegraphics[width=14.1cm,clip]{5775fg11} \end{figure}$ Figure 11: Line profiles for p=0.1 dyn cm^-2 (solid line) and p=0.01 dyn cm^-2 (dashed line), with T=8000 K and L=2000 km, at different velocities (same as in Fig. 9).
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In the text

$\begin{figure} \par\includegraphics[width=14.1cm,clip]{5775fg14} \end{figure}$ Figure 14: Line profiles for L=2000 km (solid line) and L=200 km (dashed line), with T=8000 K and p=0.1 dyn cm^-2, at different velocities (same as in Fig. 9).
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In the text

$\begin{figure} \par\includegraphics[width=8.65cm,clip]{5775fig1} \end{figure}$	Figure 1: Schematic representation of the free-standing vertical prominence slab. The slab has a geometrical extension L along the line-of-sight to the observer, at the altitude H above the limb. The prominence plasma is moving radially outwards at the velocity $\vec{V}$ .
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5775fig2} \end{figure}$	Figure 2: Angle-averaged incident profiles in the prominence frame in the He I 584 line for a prominence located at 50 000 km above the limb, and for velocities ranging from 0 (solid line) to 240 km s^-1 (step = 80 km s^-1). The incident profile is shifted towards the red when the velocity increases.
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$\begin{figure} \par\includegraphics[width=14.2cm,clip]{5775fig4} \end{figure}$	Figure 4: Same as Fig. 3, with the abscissa now in Doppler units and limited to 10 Doppler widths around line centre, and the intensities on the vertical axis now shown on a log scale. The thin solid line shows the incident line profile, gradually shifting towards the red as the prominence is moving radially upwards.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5775fig5} \end{figure}$	Figure 5: Comparison of the relative contribution of the Doppler core in the emitted line integrated intensities between CRD (dotted line) and PRD (solid line) calculations for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å( $\Diamond$ ). Same model as for Fig. 3.
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5775fig6} \end{figure}$	Figure 6: Comparison of the relative integrated intensities (integrated intensities normalised to the intensity at rest) between CRD (dotted line) and PRD (solid line) calculations for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å ( $\Diamond$ ). Same model as in Fig. 3.
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5775fig8} \end{figure}$	Figure 8: Relative intensity as a function of velocity at 8000 K (solid line) and 15 000 K (dotted line) for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å ( $\Diamond$ ).
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$\begin{figure} \par\includegraphics[width=8.05cm,clip]{5775fg10} \end{figure}$	Figure 10: Relative intensity as a function of velocity at 0.01 dyn cm^-2 (dotted line) and 0.1 dyn cm^-2 (solid line) for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å ( $\Diamond$ ).
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5775fg12} \end{figure}$	Figure 12: Population density of the ground level of He II as a function of velocity. The thickest lines refer to the mean population, the medium-thick line shows the level population at the surface of the slab, and the thinnest line corresponds to the population at slab centre. Solid lines: reference model with P=0.1 dyn cm^-2; dashed lines: low-pressure model with P=0.01 dyn cm^-2.
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$\begin{figure} \par\includegraphics[width=8.05cm,clip]{5775fg13} \end{figure}$	Figure 13: Relative intensity as a function of velocity for a slab width of 200 km (dotted line) and 2000 km (solid line) for He I $\lambda \lambda$ 584 (+) and 537 Å (*) and He II $\lambda$ 304 Å ( $\Diamond$ ).
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$\begin{figure} \par\includegraphics[width=14.1cm,clip]{5775fig9} \end{figure}$	Figure 9: Line profiles for T=8000 K (solid line) and T=15 000 K (dashed line), with p=0.1 dyn cm^-2, and L=2000 km, at different velocities: 0, 40, 80, 120, 200 and 400 km s^-1 from top to bottom. Abscissa is $\Delta \lambda$ in Å and vertical axis is specific intensity in erg s^-1 cm^-2 sr^-1 Å^-1.
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$\begin{figure} \par\includegraphics[width=14.1cm,clip]{5775fg11} \end{figure}$	Figure 11: Line profiles for p=0.1 dyn cm^-2 (solid line) and p=0.01 dyn cm^-2 (dashed line), with T=8000 K and L=2000 km, at different velocities (same as in Fig. 9).
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$\begin{figure} \par\includegraphics[width=14.1cm,clip]{5775fg14} \end{figure}$	Figure 14: Line profiles for L=2000 km (solid line) and L=200 km (dashed line), with T=8000 K and p=0.1 dyn cm^-2, at different velocities (same as in Fig. 9).
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