Line profile variations caused by low-frequency non-radial pulsations of rapidly rotating stars: II

Abstract

Line profile variations caused by low-frequency non-radial pulsations of rapidly rotating stars have been calculated, which take into account the temperature dependence of the absorption line equivalent width. Test calculations have been made for Si III 4553 A and He I 6678 A. The relative amplitude of temperature variation has been assumed to be comparable to the amplitude of velocity variation relative to the equatorial rotation velocity, which is reasonable for low-frequency oscillations because of the boundary condition