All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{3008u.ps} \end{figure}$ Figure 1: The part of the wavelength range used by the MK classification process, where the Be nature is most visible, for three early-type Be stars at different inclinations.
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In the text

$\begin{figure} \par\psfig{angle=-90,figure=3008s1.ps,width=8.8cm,clip}\par\vspace*{3mm} \psfig{angle=-90,figure=3008s2.ps,width=8.8cm,clip} \end{figure}$ Figure 2: The values of $v \sin i$ ( upper panel) and w ( lower panel) of the shell stars in Table 1 (i.e. the ones listed in the upper part) plotted against spectral subtype. While the rotational velocity depends on spectral type, but little on luminosity class, the critical fraction is largely independent of spectral type.
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In the text

$\begin{figure} \par\parbox{8cm}{ \psfig{figure=3008x2.ps,width=8.4cm,clip,angle=0} }\end{figure}$ Figure 3: Narrow absorption cores in the Fe II 5169 profile of five stars. See Table 3 for measured properties.
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In the text

$\begin{figure} \par\parbox{8.8cm}{ \parbox{4.35cm}{\psfig{figure=3008a1.ps,width... ...rbox{4.35cm}{\psfig{figure=3008a2.ps,width=4.34cm,clip,angle=0}} }\end{figure}$ Figure A.1: Evidence for $\mu$ For being a shell star. The dotted lines mark $\pm v \sin i = 320$ km ^-1. The Fe II lines show absorption cores typical of weak shells, and Si II 6347 (second profile from bottom) even exhibits a central quasi emission bump (CQE), which is formed in a Keplerian disk seen edge-on (Rivinius et al. 1999). The Mg II 4481 line shows the undisturbed stellar rotational profile for comparison. The central H $\alpha$ absorption is also very deep.

In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{3008b1.ps}\includegraphics[w... ...08b2.ps}\par\includegraphics[angle=270,width=8.2cm,clip]{3008b3.ps} \end{figure}$ Figure A.2: Shell lines of $\psi$ Per observed with H EROS in 2002. The V/R is unity for the Balmer lines, but greater than one for Fe II 5317 and less than one for Fe II 5169.

In the text

$\begin{figure} \par\psfig{angle=270,figure=3008e1.ps,width=8.4cm,clip}\par\vspac... ...} \hspace*{-4mm}\psfig{angle=270,figure=3008e3.ps,width=8.4cm,clip} \end{figure}$ Figure A.3: The evolution of the circumstellar shell Fe II lines of $\zeta$ Tau observed with F LASH/H EROS is shown in the upper panel. The spectra have an offset upwards proportional to time, except the 1991 spectrum, which is included as dashed line. The radial velocity curve of the Si II 6347 shell absorption, including also the Ondrejov data, is plotted in the middle panel. The lower panel displays He I 4713, relatively unaffected by the shell, and two dotted lines at $\pm$ $v \sin i=320$ km s^-1.

In the text

$\begin{figure} \par\psfig{angle=270,figure=3008f1.ps,width=7.7cm,clip}\par\vspace*{3mm} \psfig{angle=0,figure=3008f2.ps,width=8.5cm,clip} \end{figure}$ Figure A.4: Triple-peaked profiles in $\zeta$ Tau. The upper panel shows the spectrum taken on April 1, 1991. Note that strong telluric absorptions exist in the red part only of H $\alpha$ . The evolution of the H $\alpha$ line from 1991 to 2003 is shown in the lower panels. The vertical offset of the profiles is proportional to time and corresponds to one continuum unit per 1/4 year. The lowermost spectra were taken Apr. 1, 1991 ( left) and Aug. 19, 1998 ( right), respectively . Triple peaked profiles occur when the V/Rratio changes from <1 to >1.

In the text

$\begin{figure} \par\psfig{angle=270,figure=3008g0.ps,width=8.8cm,clip,}\par\parb... ...ip}} \parbox{4.35cm}{\psfig{figure=3008g2.ps,width=4.35cm,clip}} }\end{figure}$ Figure A.5: Upper panel: He I 6678 radial velocity curve of $\nu$ Gem (Table 2), phased with P=53.72 d. The parameters of the radial velocity curve plotted are listed in Table A.1, V ELOC solution. Open symbols mark photographic measurements taken 1983-1985 by Jarad et al. (1989). Lower panels: photospheric lines like He I 6678 are RV variable, while circumstellar shell lines like Fe II 5169 (only covered by H EROS spectra) do not follow this period, although an underlying stellar component can be seen to vary.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{figure=3008h.ps,width=8.8cm,clip} }\end{figure}$ Figure A.6: Line profiles of H $\alpha$ of $\nu$ Gem. A vertical offset of one flux unit corresponds to one year. The first spectrum was taken Nov. 2, 1994. Note the remarkable similarity of the H $\alpha$ profiles in 2002 to that of $\zeta$ Tau in 1991 (Fig. A.4). Both stars are binaries. The red peak of the late 2000 profiles is affected by strong telluric absorption.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008i.ps,width=8.8cm,clip} }\end{figure}$ Figure A.7: Radial velocity of the H $\alpha$ core of $\nu$ Gem. The circle was taken from Hummel & Vrancken (1995).

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008j.ps,width=8.8cm,clip} }\end{figure}$ Figure A.8: Mean circumstellar shell component of the spectrum of $\nu$ Gem in Fe II 5169. This spectral range is covered by H EROS data only. Note the early 2002 profile, which is similar to the Fe II profile of $\zeta$ Tau in 1991 (Fig. A.3), as are the H $\alpha$ profiles.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{figure=3008x1.ps,width=8.6cm,clip} }\end{figure}$ Figure A.9: Narrow shell lines in the UVES spectrum of $\beta$ Mon A. These lines are seen in our own F EROS data as well, but are fully resolved only by UVES. The dotted line marks the systemic radial velocity given in the GCRV, 20 km s^-1 (Wilson 1953). Narrower absorptions around the Si II 6347 line are of telluric origin.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008k1.ps,width=8.5cm... ...vspace*{3mm} \psfig{angle=270,figure=3008k2.ps,width=8.5cm,clip} }\end{figure}$ Figure A.10: Averaged profiles of spectral lines of 27 CMa in 2000. An almost uncontaminated line, indicative of a stellar $v \sin i$ of at least 300 km s ^-1 is shown in the upper panel. The lower profile has intermediate shell contribution, a typical CQE can be seen.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008l1.ps,width=8.8cm,clip} \psfig{angle=270,figure=3008l2.ps,width=8.8cm,clip} }\end{figure}$ Figure A.11: Photospheric profile ( upper panel) and sample CQE ( lower panel) of $\kappa ^1$ Aps in the 1999 season. $v \sin i=\pm350$ km s^-1 is indicated by dotted lines. Lower $v \sin i$ values may have resulted from the contamination by narrow shell absorptions.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008m.ps,width=8.8cm,clip} }\end{figure}$ Figure A.12: Evolution of the H $\alpha$ profile of $\theta$ CrB from 2000 to 2003. A vertical offset of one flux unit corresponds to one year. The first spectrum was taken May 16, 2000, the last one on Aug. 11, 2003. The mean of the 1991 Tautenburg data is shown as a dotted line for comparison. The apparent absence of telluric lines is due to the lower resolving power of R = 12 000 of this spectrum instead of 20 000 as in the later data. In the right panel the residuals are plotted w.r.t. the Tautenburg 1991 data, which is repeated for comparison.

In the text

$\begin{figure} \par\parbox{18.8cm}{ \parbox{6.1cm}{\psfig{figure=3008n1.ps,width... ...clip}} \parbox{6.1cm}{\psfig{figure=3008n3.ps,width=5.5cm,clip}} }\end{figure}$ Figure A.13: Evolution of H $\beta$ , Fe II 5169, and Na I D shell absorption in 48 Lib between 1995 and 2002.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008o.ps,width=8.8cm,clip} }\end{figure}$ Figure A.14: Periodic radial velocity variations of the H $\delta$ absorption core of $\epsilon$ Cap, sorted with P=128.5 d. The parameters for the plotted radial velocity curve are compiled in Table A.1 (V ELOC solution). Additional points were measured by us in 76 spectra taken over two weeks in Sep. 1998 by Balona (2002).

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008p.ps,width=8.8cm,clip} }\end{figure}$ Figure A.15: CQE in the Mg II 4481 profile of o Aqr in 1999.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008q.ps,width=8.8cm,clip} }\end{figure}$ Figure A.16: V/R ratio of H $\alpha$ and radial velocity of the Si II 6347 shell absorption of EW Lac. Note the strong cycle-to-cycle variations of amplitude and cycle length.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{figure=3008x4.ps,width=8.8cm,clip} }\end{figure}$ Figure B.1: V/R peak height ratios observed in Si II 6347 and He I 6678 of $\gamma$ Cas.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008x3.ps,width=8.8cm,clip} }\end{figure}$ Figure B.2: A spectrum of $\gamma$ Cas on JD = 50358, showing different V/R ratios in different lines. This indicates a trailing spiral structure of the density wave causing the V/R variations (see Appendix A about $\gamma$ Cas for detailed explanation). The red absorption wing of H $\gamma$ is blended with another Fe II emission line

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008c1.ps,width=8.8cm,clip} \psfig{angle=270,figure=3008c2.ps,width=8.8cm,clip} }\end{figure}$ Figure B.3: The changes of the emission profile of Pleione between 1991 and 2003. Note the strong variable asymmetry of the Balmer absorption wings vs. the V/R ratio of the emission, which in Fe II is ahead of H $\beta$ , while in H $\alpha$ the red peak even in 2003 is till higher than the blue one (Fig. B.4).

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{figure=3008d.ps,width=8.8cm,clip} }\end{figure}$ Figure B.4: H $\alpha$ line profiles of 28 Tau. A vertical offset of one flux unit corresponds to one year. The first spectrum was taken Jan. 8, 1991, the last one on Feb. 15, 2003. Horizontal lines mark the continua of the first and last spectra, and the one with the most pronounced red displacement of its base. Vertical lines at $\pm$ 250 km s^-1 are to visualize the secular shift of the emission base towards the red.

In the text

$\begin{figure} \par\parbox{8.8cm}{ \psfig{angle=270,figure=3008r.ps,width=8.8cm,clip} }\end{figure}$ Figure B.5: The H $\alpha$ lines of the Bn stars 1 Sco, 2 Sco, and $\eta$ Aqr observed 1999. The line cores show a CQE-like deformation, which is known also from Be stars in a weak disk state (cf. $\theta$ CrB, Fig. A.12). Several Bn stars with normal H $\alpha$ profiles are plotted in the lower part for comparison, a spectrum of $\theta$ CrB showing such a profile distortion in the upper part.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{3008u.ps} \end{figure}$	Figure 1: The part of the wavelength range used by the MK classification process, where the Be nature is most visible, for three early-type Be stars at different inclinations.
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$\begin{figure} \par\psfig{angle=-90,figure=3008s1.ps,width=8.8cm,clip}\par\vspace*{3mm} \psfig{angle=-90,figure=3008s2.ps,width=8.8cm,clip} \end{figure}$	Figure 2: The values of $v \sin i$ ( upper panel) and w ( lower panel) of the shell stars in Table 1 (i.e. the ones listed in the upper part) plotted against spectral subtype. While the rotational velocity depends on spectral type, but little on luminosity class, the critical fraction is largely independent of spectral type.
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$\begin{figure} \par\parbox{8cm}{ \psfig{figure=3008x2.ps,width=8.4cm,clip,angle=0} }\end{figure}$	Figure 3: Narrow absorption cores in the Fe II 5169 profile of five stars. See Table 3 for measured properties.
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