deletions | additions       diff --git a/Nonradial_pulsations_have_also.tex b/Nonradial_pulsations_have_also.tex  index d4e3621..35715c7 100644  --- a/Nonradial_pulsations_have_also.tex  +++ b/Nonradial_pulsations_have_also.tex 
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components \cite{1988MNRAS.233..123P,1995ApJ...452L..53M,1997A&A...327..281K,2002A&A...388..587P}  at the surface or in the wind of massive OB stars.  Non-radial g-mode pulsations were also recently proposed as the origin  of observable macroturbulence in massive B~type stars \citep{2008arXiv0812.2641A}. \cite{2008arXiv0812.2641A}.  In Fig.~\ref{pulsationplot} we compare the regions where strange mode, g-mode,   and p-mode pulsations are predicted to occur in the HR diagram   with the region where our models predict a strong FeCZ.   Pulsations appear to be almost ubiquitous when all types of variables are accounted  for. The strange mode pulsators are predicted to cover the HR diagram at high  luminosity, where we plotted only the predictions for the radial strange modes of \citet{1993MNRAS.264...50K}; \cite{1993MNRAS.264...50K};  high-order non-radial strange modes seem to be omnipresent  as well for stars above 40$\mso$ or so \citep{1996MNRAS.282.1470G}. \cite{1996MNRAS.282.1470G}.  Non-radial g-mode pulsators are predicted by \citet{2006ApJ...650.1111S} \cite{2006ApJ...650.1111S}  in the B~supergiant region. And radial and low order non-radial p-modes are predicted for the  $\beta\,$Cephei regime by \citet{2001MNRAS.327..881D} \cite{2001MNRAS.327..881D}  and by \citet{1999AcA....49..119P} \cite{1999AcA....49..119P}  and At lower metallicity, many of the predicted areas in the HR diagram are   smaller \citep[cf.,][]{1993MNRAS.264...50K, \cite{1993MNRAS.264...50K,  2001MNRAS.327..881D} but the general picture is still incomplete.