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