Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig1.eps}} \end{figure}$ Figure 1: Molecular potentials for H₂ correlated to the 3d and 2p singlet states of atomic H. The energies from Spielfiedel et al. (2004) are given relative to the asymptotic atomic state. See Table 4 for transition identifications.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig2.eps}} \end{figure}$ Figure 2: Molecular potentials for H₂ correlated to the 3d and 2p triplet states of atomic H. The energies from Spielfiedel et al. (2004) are given relative to the asymptotic atomic state. See Table 4 for transition identifications.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8437fig3.eps} \end{figure}$ Figure 3: Variation of the line width (HWHM) per perturber with temperature for the 6 strongest transitions of the 3d-2p component.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8437fig4.eps} \end{figure}$ Figure 4: Potential difference for the 6 strongest transitions of the 3d-2p component.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig5.eps}} \end{figure}$ Figure 5: Potential difference for the j-c and du-i triplet transitions contributing to Balmer $\alpha$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig6.eps}} \end{figure}$ Figure 6: Potential difference for the k-a and r-f triplet transitions contributing to Balmer $\alpha$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig7.eps}} \end{figure}$ Figure 7: Comparison of the line width of the contributions of the different components, 3d-2p, 3p-2s and 3s-2p, due to H-H collisions with temperature in the different approaches using a single velocity $\bar{v}$ and averaging over velocity. (--) Total of all contributions averaged over velocity; ( $\circ~\circ~\circ$ ) total using $\bar{v}$ ; ( $-\cdot \cdot -\cdot \cdot -$ ) 3d-2p only, averaged over velocity; ( $\Box$ ) 3d-2p only, using $\bar{v}$ ; (- - -) 3p-2s only, averaged over velocity; ( $\Diamond$ ) 3p-2s only, using $\bar{v}$ ; ( $\cdot \cdot \cdot$ ) 3s-2p only, averaged over velocity; ( $\bigtriangleup$ ) 3s-2p only, using $\bar{v}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig8.eps}} \end{figure}$ Figure 8: Comparison of the line shift of the contributions of the different components, 3d-2p, 3p-2s and 3s-2p, due to H-H collisions with temperature in the different approaches using a single velocity $\bar{v}$ and averaging over velocity. Same symbols as in Fig. 7. (--) Total of all contributions averaged over velocity; ( $\circ~\circ~\circ$ ) total using $\bar{v}$ ; ( $-\cdot \cdot -\cdot \cdot -$ ) 3d-2p only, averaged over velocity; ( $\Box$ ) 3d-2p only, using $\bar{v}$ ; (- - -) 3p-2s only, averaged over velocity; ( $\Diamond$ ) 3p-2s only, using $\bar{v}$ ; ( $\cdot \cdot \cdot$ ) 3s-2p only, averaged over velocity; ( $\bigtriangleup$ ) 3s-2p only, using $\bar{v}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig9.eps}} \end{figure}$ Figure 9: Comparison of the line width of the contributions of the singlets and triplets to the 3d-2p component of H $\alpha$ . (--) 3d-2p averaged over velocity; ( $\Box$ ) 3d-2p, using $\bar{v}$ ; (- - -) 3d-2p triplets only, averaged over velocity; ( $\circ$ ) 3d-2p triplets only using $\bar{v}$ ; ( $\cdot \cdot \cdot$ ) 3d-2p singlets only, averaged over velocity; ( $\Diamond$ ) 3d-2p singlets only, using $\bar{v}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig10.eps}} \end{figure}$ Figure 10: Comparison of the line width due to H-H collisions with temperature in the different approaches. (--) Total of all contributions averaged over velocity; (- - -) Barklem et al. (2000b); ( $\cdot \cdot \cdot$ ) Ali & Griem (1966); ( $\circ$ ) total using $\bar{v}$ ; ( $-\cdot \cdot -\cdot \cdot -$ ) 3d-2p only, averaged over velocity; ( $\Box$ ) 3d-2p only, using $\bar{v}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig11.eps}} \end{figure}$ Figure 11: Total unified line profile compared to the Lorentzian profile. (T=4000 K, $n_{{\rm H}}=1\times 10^{18}$ cm^-3).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[width=10cm]{8437fig12.eps}} \end{figure}$ Figure 12: Comparison of the theoretical profiles of H $_{\alpha }$ with the observed solar spectrum. Using the solar MARCS model.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[width=10cm]{8437fig13.eps}} \end{figure}$ Figure 13: Comparison of the theoretical profiles of H $_{\alpha }$ with the observed solar spectrum. Using the Holweger-Müller model.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig1.eps}} \end{figure}$	Figure 1: Molecular potentials for H₂ correlated to the 3d and 2p singlet states of atomic H. The energies from Spielfiedel et al. (2004) are given relative to the asymptotic atomic state. See Table 4 for transition identifications.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig2.eps}} \end{figure}$	Figure 2: Molecular potentials for H₂ correlated to the 3d and 2p triplet states of atomic H. The energies from Spielfiedel et al. (2004) are given relative to the asymptotic atomic state. See Table 4 for transition identifications.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{8437fig3.eps} \end{figure}$	Figure 3: Variation of the line width (HWHM) per perturber with temperature for the 6 strongest transitions of the 3d-2p component.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{8437fig4.eps} \end{figure}$	Figure 4: Potential difference for the 6 strongest transitions of the 3d-2p component.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig5.eps}} \end{figure}$	Figure 5: Potential difference for the j-c and du-i triplet transitions contributing to Balmer $\alpha$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig6.eps}} \end{figure}$	Figure 6: Potential difference for the k-a and r-f triplet transitions contributing to Balmer $\alpha$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig10.eps}} \end{figure}$	Figure 10: Comparison of the line width due to H-H collisions with temperature in the different approaches. (--) Total of all contributions averaged over velocity; (- - -) Barklem et al. (2000b); ( $\cdot \cdot \cdot$ ) Ali & Griem (1966); ( $\circ$ ) total using $\bar{v}$ ; ( $-\cdot \cdot -\cdot \cdot -$ ) 3d-2p only, averaged over velocity; ( $\Box$ ) 3d-2p only, using $\bar{v}$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{8437fig11.eps}} \end{figure}$	Figure 11: Total unified line profile compared to the Lorentzian profile. (T=4000 K, $n_{{\rm H}}=1\times 10^{18}$ cm^-3).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[width=10cm]{8437fig12.eps}} \end{figure}$	Figure 12: Comparison of the theoretical profiles of H $_{\alpha }$ with the observed solar spectrum. Using the solar MARCS model.
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$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[width=10cm]{8437fig13.eps}} \end{figure}$	Figure 13: Comparison of the theoretical profiles of H $_{\alpha }$ with the observed solar spectrum. Using the Holweger-Müller model.
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