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We determine instability domains on the Hertzsprung-Russel diagram forrotating main sequence stars with masses 2-20 $\mathrm M_\odot$. The effects ofthe Coriolis force are treated in the framework of the traditionalapproximation. High-order g-modes with the harmonic degrees, $\ell$, up to 4and mixed gravity-Rossby modes with $|m|$ up to 4 are considered. Including theeffects of rotation results in wider instability strips for a given $\ell$comparing to the non-rotating case and in an extension of the pulsationalinstability to hotter and more massive models. We present results for the fixedvalue of the initial rotation velocity as well as for the fixed ratio of theangular rotation frequency to its critical value. Moreover, we check how theinitial hydrogen abundance, metallicity, overshooting from the convective coreand the opacity data affect the pulsational instability domains. The effect ofrotation on the period spacing is also discussed.

Domains of pulsational instability of low-frequency modes in rotating upper main-sequence stars