In Sect. \ref{magnetic}, we proposed that the FeCZ in hot stars might also produce localized surface magnetic fields, in Galactic stars for luminosities above \(\sim 10^{3.2}{\,{\rm L}_\odot}\). This could explain the occurrence of DACs (discrete absorption components in UV absorption lines), also in very hot main sequence stars for which pulsational instabilities are not predicted. We further argued that there may be regions of the upper HR diagram for which the presence of the FeCZ influences, or even excites, non-radial stellar pulsations (Sect. \ref{pulsation}).