We have examined whether the kappa-mechanism at the ”Z” opacity bump can excite overstable nonradial pulsation (NRP) modes such as those responsible for the line-profile variations (lpv) observed for ϵ Persei (Gies et al. 1999).
From the lpv modeling with realistic stellar parameters and the state-of-the-art codes, we confirmed that the observed lpv can generally be explained by the modes with l values suggested by Gies et al. (1999). We have also found that some tesseral modes, which have smaller m than those of sectoral modes, can reproduce the observed lpv well for the periods of 3.51hr/3.84 hr and 4.06hr/4.54 hr. Our linear non-adiabatic nonradial pulsation analysis applied to massive (13M⊙––14M⊙) stars shows that the periods of higher |m| values in the co-rotating frame are too long to be excited by the Z-bump kappa-mechanism while the smaller |m| values give marginal consistency.