All Tables

Table 1: The shell stars considered in this study and their observed parameters. Unless otherwise noted here or in Sect. 3, Sp. type and $v \sin i$ were taken from Slettebak (1982), but always cross-checked against our data where possible. w was calculated using $v_{\rm crit}$ given in Table 2 of Yudin (2001), who interpolated values by Moujtahid et al. (1999). For stars without available luminosity class, the $v_{\rm crit}$ for dwarfs was used to obtain a lower limit to w. Since Sect. 4.3 relies on simultaneously obtained data for a given star, the columns for V/R variability and CQE only list the state of the disk during our observations, although such information is available from the literature also for other times and the other stars.
Table 2: Line parameters for $\nu$ Gem: Next to the heights (in continuum units) of the V and R emission peaks the one of the central peak is given, when a triple-peaked profile was present (C peak). The radial velocities correspond to the local minima (modes) in these lines (for H $\alpha$ of the central depression). The typical error is 11 and 3 km s ^-1 for the He I 6678 measurements in the Ondrejov coudé and H EROS data, respectively, and about 1 and 0.2 km s ^-1 for the much sharper H $\alpha$ absorption core. The full table and similar tables for other stars are published electronically only.
Table 3: Properties of the narrow cores observed in the Fe II 5169 lines of five shell stars. The resolving power of UVES was R=80 000, see Sect. 2 for H EROS and F EROS. The stellar radial velocities $v_\star$ were taken from the General Catalogue of Radial Velocities (Wilson 1953, GCRV) and its revised edition (Evans 1967), respectively. All numbers are given in km s^-1.
Table A.1: Binary parameters derived from the radial velocities (RVs) of $\nu$ Gem (Fig. A.5) and $\epsilon$ Cap (Fig. A.14) by means of V ELOC (Schmutz, unpublished, e.g. used also by Schmutz et al. 1997) and F OTEL (Hadrava 2002). Since the eccentricity is zero for $\epsilon$ Cap, T₀ denotes the time of maximal RV. The V ELOC and F OTEL solutions agree very well within their errors.