Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=90,width=6.6cm]{h4197_1.eps}\par\includegraphics[angle=90,width=6.7cm]{h4197_2.eps}\end{figure}$ Figure 1: Upper: HR 2020, obtained on 2002 Mar. 25, UT 23:37 (solid line), on 2002 Mar. 26, UT 23:25 (dashed line), and on 1996 Feb. 29, UT 00:11 (dashed-dotted line). Note the nightly variation at $\sim$ 8 km s^-1 in the 2002 spectra. Lower: redward line wing of HR 2020 on 2002 Mar. 25, UT 23:37 (solid line). For comparison, the high velocity feature detected in the second night is shown. Dashed line: 2002 Mar. 26, UT 23:25, dotted line: 2002 Mar. 27, UT 01:19. The radial velocity with respect to the star of this feature corresponds to $v_{\rm K}~\approx100$ km s^-1 and $v_{\rm K}~\approx110$ km s^-1, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm]{h4197_3.eps}\end{figure}$ Figure 2: HR 2550 recorded on 2002 Mar. 26, UT 00:33 (solid line) and 1996 Feb. 29, UT 01:24 (dashed line). Note the change of the radial velocity of the absorption feature in the line core.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm]{h4197_4.eps}\end{figure}$ Figure 3: The Ca II K line of HR 3685 recorded on 2002 Mar. 26, UT 00:13 (solid line) and 1996 Feb. 29, UT 03:30 (dashed line). The feature changed in both radial velocity and shape.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm]{h4197_5.eps}\\ [0mm] \end{figure}$ Figure 4: Spectra of HR 3485 obtained on 2002 Mar. 26, UT 00:07 (solid line) and 1996 Feb. 28, UT 05:09 (dashed line). The features do not show any long-term variability.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{h4197_6.eps}\end{figure}$ Figure 5: HR 4796 obtained on 2002 Mar. 26, UT 02:44 (solid line) and 1996 Feb. 29, UT 03:43 (dashed line). Despite the presence of circumstellar dust no signs of variable gas motions are detectable.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{h4197_7.eps}\end{figure}$ Figure 6: The $\lambda$ Bootis star HR 4881 obtained on 2002 Mar. 26, UT 03:50; (solid line) and 1996 Feb. 28, UT 07:40 (dashed line). The change of the radial velocity of the narrow absorption feature can be ascribed to the binarity of HR 4881.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{h4197_8.eps}\end{figure}$ Figure 7: HR 5367 on 2002 Mar. 26, UT 06:24 (solid line) and 1997 Sep. 15, UT 23:57 (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm]{h4197_9.eps}\end{figure}$ Figure 8: HR 6519 on 2002 Mar. 26, UT 08:20 (solid line) and 1996 Feb. 29, UT 09:15 (dashed-dotted line). The advantage of the higher spectral resolution is obvious. For comparison, the dashed line shows the 2002 spectrum degraded to the resolution of our 1996 data.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{h4197_10.eps}\end{figure}$ Figure 9: Spectra of HR 6556 recorded on 2002 Mar. 26, UT 09:08 (solid line) and 1996 Feb. 29, UT 09:15 (dashed line). The extraordinary strong absorption feature of the nearest star in our sample is stable for years.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm]{h4197_3.eps}\end{figure}$	Figure 2: HR 2550 recorded on 2002 Mar. 26, UT 00:33 (solid line) and 1996 Feb. 29, UT 01:24 (dashed line). Note the change of the radial velocity of the absorption feature in the line core.
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$\begin{figure} \par\includegraphics[width=6.6cm]{h4197_4.eps}\end{figure}$	Figure 3: The Ca II K line of HR 3685 recorded on 2002 Mar. 26, UT 00:13 (solid line) and 1996 Feb. 29, UT 03:30 (dashed line). The feature changed in both radial velocity and shape.
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$\begin{figure} \par\includegraphics[width=6.6cm]{h4197_5.eps}\\ [0mm] \end{figure}$	Figure 4: Spectra of HR 3485 obtained on 2002 Mar. 26, UT 00:07 (solid line) and 1996 Feb. 28, UT 05:09 (dashed line). The features do not show any long-term variability.
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$\begin{figure} \par\includegraphics[width=7cm]{h4197_6.eps}\end{figure}$	Figure 5: HR 4796 obtained on 2002 Mar. 26, UT 02:44 (solid line) and 1996 Feb. 29, UT 03:43 (dashed line). Despite the presence of circumstellar dust no signs of variable gas motions are detectable.
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$\begin{figure} \par\includegraphics[width=7cm]{h4197_7.eps}\end{figure}$	Figure 6: The $\lambda$ Bootis star HR 4881 obtained on 2002 Mar. 26, UT 03:50; (solid line) and 1996 Feb. 28, UT 07:40 (dashed line). The change of the radial velocity of the narrow absorption feature can be ascribed to the binarity of HR 4881.
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$\begin{figure} \par\includegraphics[width=7cm]{h4197_8.eps}\end{figure}$	Figure 7: HR 5367 on 2002 Mar. 26, UT 06:24 (solid line) and 1997 Sep. 15, UT 23:57 (dashed line).
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$\begin{figure} \par\includegraphics[width=6.1cm]{h4197_9.eps}\end{figure}$	Figure 8: HR 6519 on 2002 Mar. 26, UT 08:20 (solid line) and 1996 Feb. 29, UT 09:15 (dashed-dotted line). The advantage of the higher spectral resolution is obvious. For comparison, the dashed line shows the 2002 spectrum degraded to the resolution of our 1996 data.
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$\begin{figure} \par\includegraphics[width=7cm]{h4197_10.eps}\end{figure}$	Figure 9: Spectra of HR 6556 recorded on 2002 Mar. 26, UT 09:08 (solid line) and 1996 Feb. 29, UT 09:15 (dashed line). The extraordinary strong absorption feature of the nearest star in our sample is stable for years.
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