All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5891f1a.eps}\par\vspace*{2mm} \includegraphics[width=6.5cm,clip]{5891f1b.eps}\end{figure}$ Figure 1: HD 209458b atmospheric model. Upper panel: temperature profile in the atmosphere of the planet HD 209458b; from Yelle (2004). Lower panel: density profiles of H (solid line) and H₂ (dashed line) in the atmosphere of HD 209458b; from Yelle (2004).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{5891f2a.eps}\par {\hspace*{5mm}\includegraphics[width=5.8cm,clip]{5891f2b.eps}\hspace*{5mm}} \end{figure}$ Figure 2: Lyman $\alpha$ ( upper panel) and Lyman $\beta$ ( lower panel) line profile from the star with or without a transit with a 25 000 km thick H₂ layer. The diminution of the total intensity is 10.45% in the Lyman $\alpha$ case, and 10.53% in the Lyman $\beta$ case. The difference is consistent with the fact that Lyman $\beta$ has a single scattering albedo equal to 0.86 lower than the Lyman $\alpha$ single scattering albedo, equal to 1. No effect of the H₂ lines is visible.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{5891f3.eps}\end{figure}$ Figure 3: Ratio of the Lyman $\alpha$ line profile during a transit with the H₂ layer divided by the line profile without the H₂ layer.
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In the text

$\begin{figure} \par {\hspace*{5mm}\includegraphics[width=5.8cm,clip]{5891f4a.eps}\hspace*{5mm}} \par\includegraphics[width=6.8cm,clip]{5891f4b.eps}\end{figure}$ Figure 4: Planetary emission in the Lyman $\alpha$ ( upper panel) and Lyman $\beta$ cases ( lower panel) for several vibrational temperatures (1 and 4 times the kinetic ones). The lack of symmetry is very faint in the case of Lyman $\alpha$ and strong in the case of Lyman $\beta$ . In the two panels, the solid line corresponds to $T_{\rm vib}=T_{\rm kin}$ . The dotted line corresponds to $T_{\rm vib}=4T_{\rm kin}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{5891f5.eps}\end{figure}$ Figure 5: Stellar C III line in a situation just before an transit (solid line) and during the transit with an H₂ layer 25 000 km thick (dashed line) and with an H₂ layer 100 000 km thick (dotted line). The wavelength centre of the C III line is at 977.02 Å. The bottom lines represent the difference between the two curves (25 000 km for the crosses, 100 000 km for the triangles).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5891f6.eps} \end{figure}$ Figure 6: Emission of the planet in the region of the C III line in a geometry similar to the Fig. 4, i.e. with a maximum angular separation.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5891f1a.eps}\par\vspace*{2mm} \includegraphics[width=6.5cm,clip]{5891f1b.eps}\end{figure}$	Figure 1: HD 209458b atmospheric model. Upper panel: temperature profile in the atmosphere of the planet HD 209458b; from Yelle (2004). Lower panel: density profiles of H (solid line) and H₂ (dashed line) in the atmosphere of HD 209458b; from Yelle (2004).
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{5891f3.eps}\end{figure}$	Figure 3: Ratio of the Lyman $\alpha$ line profile during a transit with the H₂ layer divided by the line profile without the H₂ layer.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{5891f5.eps}\end{figure}$	Figure 5: Stellar C III line in a situation just before an transit (solid line) and during the transit with an H₂ layer 25 000 km thick (dashed line) and with an H₂ layer 100 000 km thick (dotted line). The wavelength centre of the C III line is at 977.02 Å. The bottom lines represent the difference between the two curves (25 000 km for the crosses, 100 000 km for the triangles).
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5891f6.eps} \end{figure}$	Figure 6: Emission of the planet in the region of the C III line in a geometry similar to the Fig. 4, i.e. with a maximum angular separation.
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