deletions | additions       diff --git a/Observationally_the_classical_betaCephei.tex b/Observationally_the_classical_betaCephei.tex  index eee4d4f..24466a1 100644  --- a/Observationally_the_classical_betaCephei.tex  +++ b/Observationally_the_classical_betaCephei.tex 
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Observationally, the classical $\beta\,$Cephei stars are concentrated in the  region predicted by Deng \& Xiong \cite{2005ApJS..158..193S}, while the  B~supergiant non-radial g-mode pulsators overlap with the prediction of \cite{2006ApJ...650.1111S}  but extend to an effective temperature of $\sim 10\, 000\,$K \cite{2007A&A...463.1093L}. \cite{2007AA...463.1093L}.  Pulsations are also found for the most luminous stars \cite{1998A&AS..128..117V}, \cite{1998AAS..128..117V},  but there is now no clear evidence for strange mode pulsators.   Comparing the prediction for the FeCZ   with that for pulsational instability  (Fig.\ref{pulsationplot}) (Fig.\ref{fig:pulsationplot})  shows two things. Firstly, the FeCZ-region is much larger than any region for a particular pulsational instability. Thus, distinguishing whether a certain observational  feature is caused by a particular pulsational instability by the FeCZ might, in principle,  be possible, since the area in the HR diagram where the latter occurs but