|
Constraints on angular numbers of pulsation modes from spectroscopy John Telting, Wrocław, June 2008 |
|
||||||||
|
|
|
||||||||||||
The bright B1V star ω
Sco, rotational velocity Vsin(i)= 100 km/s,
Vmag = 3.9 with main mode L = |M| = 9
(Berdyugina et al. 2003). Hence ω
Sco is a β Cephei star.
About 50% of all bright non-emission-line
stars with spectral type in the β Cep domain show wiggles in
their line profiles (Telting et al. 2006).