Studies of line profile variability of the ultraviolet 1550 Å resonance transitions of C IV in Be stars have prompted an investigation into the short- and long-term behavior of the C IV lines in other types of B stars. The authors present examples of two well-studied Be stars, Omega Orionis and 66 Ophiuchi, and two non-Be stars, Beta Cephei and the standard star Zeta Cassiopeiae.
IAU Colloq. 92: Physics of Be Stars
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