All Figures

$\begin{figure} \par {\resizebox{0.48\textwidth}{!}{ \includegraphics*{h4496F1.ps}} }\end{figure}$ Figure 1: The 995 Å-region Lyman $\gamma$ wing. The individual contribution of the two transitions that give rise to the two main satellites are over-plotted. $I_\omega$ is the normalized line profile proportional to the absorption coefficient as described by Allard et al. (1999).
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In the text

$\begin{figure} \par {\resizebox{\textwidth}{!}{ \includegraphics*{h4496F2.ps}} }\end{figure}$ Figure 2: A comparison of the FUSE spectra of the white dwarfs and the theoretical models. Top to bottom: Wolf 1346, EG 102, BPM 6502, and CD $~-38^{\circ}10980$ . The flux is in erg/cm²/s/Å. The Lyman $\beta$ satellites are at 1058 Å and 1076 Å; the Lyman $\gamma$ satellites (enlarged in right panel) are at 992 Å and 996 Å. The narrow emission features are due to terrestrial airglow.
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In the text

$\begin{figure} \par\resizebox{0.48\textwidth}{!}{\includegraphics*{h4496F3.ps}} \end{figure}$ Figure 3: Total profile of Lyman $\alpha$ , Lyman $\beta$ , and Lyman $\gamma$ perturbed by neutral hydrogen and protons. Two different neutral densities ( $1\times 10^{16}$ cm^-3 and $5\times 10^{16}$ cm^-3) are compared for a fixed ion density ( $1\times 10^{16}$ cm^-3), and T=25 000 K. Lyman $\gamma$ profile is only perturbed by protons.
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In the text

$\begin{figure} \par {\resizebox{0.48\textwidth}{!}{ \includegraphics*{h4496F1.ps}} }\end{figure}$	Figure 1: The 995 Å-region Lyman $\gamma$ wing. The individual contribution of the two transitions that give rise to the two main satellites are over-plotted. $I_\omega$ is the normalized line profile proportional to the absorption coefficient as described by Allard et al. (1999).
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$\begin{figure} \par {\resizebox{\textwidth}{!}{ \includegraphics*{h4496F2.ps}} }\end{figure}$	Figure 2: A comparison of the FUSE spectra of the white dwarfs and the theoretical models. Top to bottom: Wolf 1346, EG 102, BPM 6502, and CD $~-38^{\circ}10980$ . The flux is in erg/cm²/s/Å. The Lyman $\beta$ satellites are at 1058 Å and 1076 Å; the Lyman $\gamma$ satellites (enlarged in right panel) are at 992 Å and 996 Å. The narrow emission features are due to terrestrial airglow.
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$\begin{figure} \par\resizebox{0.48\textwidth}{!}{\includegraphics*{h4496F3.ps}} \end{figure}$	Figure 3: Total profile of Lyman $\alpha$ , Lyman $\beta$ , and Lyman $\gamma$ perturbed by neutral hydrogen and protons. Two different neutral densities ( $1\times 10^{16}$ cm^-3 and $5\times 10^{16}$ cm^-3) are compared for a fixed ion density ( $1\times 10^{16}$ cm^-3), and T=25 000 K. Lyman $\gamma$ profile is only perturbed by protons.
Open with DEXTER