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.
HD HR name Sp. type $v \sin i$ $w\sin i$ V/R CQE binary References
number number     [km s-1]   variable occurrence    
Conventional shell stars (Appendix A)
10 516 496 $\phi$ Per B1.5 (V:)e shell 450 0.90: $\surd$ - $\surd$ 1
13 709 652 $\mu $ For A0 V 320 0.82 - $\surd$ - 2
22 192 1087 $\psi $ Per B5 IIIe shell 280 0.90 ? - -  
35 165 1772   B5 IVnp 280 0.73 no own spectra 3,4
37 202 1910 $\zeta $ Tau B1 IVe shell 320 0.66 $\surd$ - $\surd$ 5
41 335 2142   B2 IVe 350 0.79 $\surd$ - $\surd$  
45 542 2343 $\nu $ Gem B B8 IIIe - - $\surd$ - $\surd$  
45 725 2356 $\beta $ Mon A B4 Ve shell 300 0.68 - $\surd$ -  
47 760 2451 $\nu $ Pup B8 III 230 0.84 - - - 6
56 014 2745 27 CMa B3 III(e)p shell 280 0.82 - $\surd$ - 7
89 080 4037 $\omega$ Car B8 IIIe shell 220 0.80 - $\surd$ -  
91 120 4123   B9 IVe 250 0.73 - ? -  
93 563 4221   B8 III(e) shell 280 1.02 - - -  
110 335 4823 39 Cru B6 IVe 250 0.67 - - -  
127 972 5440 $\eta $ Cen B2 IV(e) 350 0.79 - $\surd$ -  
137 387 5730 $\kappa ^1$ Aps B3 IVe - 2 sp.? 350 0.83 - $\surd$ -  
138 749 5778 $\theta $ CrB B6 III 320 1.08 - $\surd$ -  
142 926 5938 4 Her B7 IVe shell 300 0.83 - $\surd$ $\surd$  
142 983 5941 48 Lib B3: IV:e shell 400 0.95: $\surd$ - -  
162 732 6664 88 Her B6 IVe 300 0.80 - - $\surd$ 8,9
183 656 7415   B6e shell 300 >0.73 no own spectra  
193 182     B8.5 III 200 0.73 no own spectra 10
195 325 7836 1 Del B8-9:(e) shell 280: >0.71: no own spectra  
205 637 8260 $\epsilon $ Cap B3 IIIe 250 0.74 - $\surd$ $\surd$  
209 409 8402 o Aqr B7 IIIe shell 300 1.06 - $\surd$ -  
217 050 8731 EW Lac B3: IV:e shell 300 0.71: $\surd$ - -  
217 675 8762 o And B6 III 260 0.88 - $\surd$ $\surd$  
Be stars having had both shell and emission phases (Appendix B)
5394 264 $\gamma $ Cas B0.5 IVe 380 0.76 $\surd$ - $\surd$ 11
23 862 1180 28 Tau B8 (V:)e shell 320 0.81: $\surd$ - -  
200 120 8047 59 Cyg B1 Ve $\ge$379 $\ge$0.73 $\surd$ - $\surd$ 7
Bn stars showing weak edge-on disk evidence (Appendix C)
141 637 5885 1 Sco B3 V 225 0.49 - $\surd$ - 12
142 114 5904 2 Sco B2.5 Vn 250 0.53 - $\surd$ - 12
213 998 8597 $\eta $ Aqr B9 IV-Vn 245 0.68 - $\surd$ - 12
1: Poeckert (1981), 2: Royer et al. (2002), 3: Hiltner et al. (1969), 4: Balona (1995), 5: Yang et al. (1990), 6: Rivinius et al. (1999), 7: Chauville et al. (2001), 8: Divan & Zorec (1982), 9: Slettebak (1976), 10: Denizman et al. (1993), 11: Harmanec (2002), 12: Abt et al. (2002).

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