Astronomy & Astrophysics

$\begin{figure} \par\rotatebox{0}{\resizebox{8.3cm}{!}{\includegraphics{1460fig01.ps}}}\end{figure}$ Figure 1: The peculiar shape of the Mg II line near 4481 Å in the spectrum of HD 4881. Four Si II lines (4128, 4130, 6347, 6371 Å) and a Ca II line (3933 Å) show a similar profile.
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In the text

$\begin{figure} \par\rotatebox{0}{\resizebox{8.3cm}{!}{\includegraphics{1460fig02.ps}}}\end{figure}$ Figure 2: The elemental abundances of AB Aur and HD 100546 determined in the present analysis compared to those of $\lambda$ Boo (Venn & Lambert 1990). The depletion pattern of HD 100546 and $\lambda$ Boo are clearly similar. This is less obvious for AB Aur. In the lower left corner, the typical $\pm 0.20$ dex error bar is shown.
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In the text

$\begin{figure} \par\rotatebox{0}{\resizebox{8cm}{!}{\includegraphics{1460fig03.ps}}}\end{figure}$ Figure 3: The elemental abundances of HD 4881 and HD 139614 determined in the present analysis. Both patterns display an overall underabundance of -0.65 dex for HD 4881 and -0.22 dex for HD 139614. In the lower right corner, the typical $\pm 0.20$ dex error bar is shown.
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In the text

$\begin{figure} \par\rotatebox{0}{\resizebox{7.7cm}{!}{\includegraphics{1460fig04.ps}}}\end{figure}$ Figure 4: The spectra of HD 28978 ( top), an A2 star with $T_{{\rm e}}=9250$ K, and HD 190073 ( bottom), are very similar. The agreement between both spectra confirms our lower - with respect to other authors - effective temperature for HD 190073.
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In the text

$\begin{figure} \par\rotatebox{0}{\resizebox{8.3cm}{!}{\includegraphics{1460fig01.ps}}}\end{figure}$	Figure 1: The peculiar shape of the Mg II line near 4481 Å in the spectrum of HD 4881. Four Si II lines (4128, 4130, 6347, 6371 Å) and a Ca II line (3933 Å) show a similar profile.
Open with DEXTER

$\begin{figure} \par\rotatebox{0}{\resizebox{8.3cm}{!}{\includegraphics{1460fig02.ps}}}\end{figure}$	Figure 2: The elemental abundances of AB Aur and HD 100546 determined in the present analysis compared to those of $\lambda$ Boo (Venn & Lambert 1990). The depletion pattern of HD 100546 and $\lambda$ Boo are clearly similar. This is less obvious for AB Aur. In the lower left corner, the typical $\pm 0.20$ dex error bar is shown.
Open with DEXTER

$\begin{figure} \par\rotatebox{0}{\resizebox{8cm}{!}{\includegraphics{1460fig03.ps}}}\end{figure}$	Figure 3: The elemental abundances of HD 4881 and HD 139614 determined in the present analysis. Both patterns display an overall underabundance of -0.65 dex for HD 4881 and -0.22 dex for HD 139614. In the lower right corner, the typical $\pm 0.20$ dex error bar is shown.
Open with DEXTER

$\begin{figure} \par\rotatebox{0}{\resizebox{7.7cm}{!}{\includegraphics{1460fig04.ps}}}\end{figure}$	Figure 4: The spectra of HD 28978 ( top), an A2 star with $T_{{\rm e}}=9250$ K, and HD 190073 ( bottom), are very similar. The agreement between both spectra confirms our lower - with respect to other authors - effective temperature for HD 190073.
Open with DEXTER