I will discuss predictions from linear oscillation calculations regarding mode excitation in the main-sequence variables of Cephei, SPB and Scuti-type. The updated instability ranges in frequency and spherical harmonic degree will be presented. Slow or moderate rotation does not influence the excitation of pulsations but it widenes the frequency range due to rotational splitting. Main uncertainties in determination of the theoretical frequency ranges for Delta Scuti models are due to inadequate treatment of convection. I will compare theoretical predictions of equidistant separations in frequency spectra with observational evidences in pulsating stars. In this context I will consider the role of mode trapping in evolved stars. In greater details I will review structures of rotationally split multiplets for the low-order modes excited in Scuti stars and for the high-order ones in solar-type stars. Also I will briefly discuss how rotation couples modes of different degrees which leads to complication in usage of the amplitude ratio – phase difference diagrams.

 
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