Astronomy & Astrophysics

$\begin{figure} \par\resizebox{65mm}{!}{\rotatebox{0}{\includegraphics{Fg171_f1a.... ...r\resizebox{65mm}{!}{\rotatebox{0}{\includegraphics{Fg171_f1b.eps}}}\end{figure}$ Figure 1: Departure coefficients with standard optical depth for lower Li I levels in the solar 1D model with $\log \epsilon_{\rm Li}=1.1$ (upper panel) and in the HD 140283 1D model with $\log \epsilon_{\rm Li}=1.8$ (lower panel). Full lines are for the atomic model without H collisions noH and the dashed lines are with H collisions wH.
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In the text

$\begin{figure} \par\resizebox{65mm}{!}{\rotatebox{0}{\includegraphics{Fg171_f1a.... ...r\resizebox{65mm}{!}{\rotatebox{0}{\includegraphics{Fg171_f1b.eps}}}\end{figure}$	Figure 1: Departure coefficients with standard optical depth for lower Li I levels in the solar 1D model with $\log \epsilon_{\rm Li}=1.1$ (upper panel) and in the HD 140283 1D model with $\log \epsilon_{\rm Li}=1.8$ (lower panel). Full lines are for the atomic model without H collisions `noH` and the dashed lines are with H collisions `wH`.
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