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tokens: in the parlance of the General Catalogue of Variable Stars. 1 The first-order combination terms between the modes n and n ′ have the following frequencies: and Given negligible first-order corrections ε T f (1, 0) , equations ( 15 ) are consistent with equations ( 4 ) and ( 7 ), while equations ( 14 ) with equations ( 8 ). The referee has suggested a test that our f n ,0 and modes are indeed associated with the l = 1, m = 0 spherical harmonics and provided examples of applying the test to simulated data. The test consists in dividing the data into two parts according to the orbital phase in such a way that one part contains the data covering orbital phases from one quadrature to the other, and the second part, the remaining data, and then computing amplitude spectra for the two parts separately. Using simulated l = 1, m = 0 light curves with an assumed pulsation frequency, Reed, Brondell Kawaler ( 2005 ) found for a range of inclination of the pulsation axis to the line of sight that in the amplitude spectra of the two parts of the data there appears a peak at the assumed frequency flanked by f orb aliases, whereas in the amplitude spectrum of the complete data set the peak at the assumed frequency is missing (see their fig. 4). In addition, there is a phase difference equal to between the light curves in the two parts of the data. For the test, we used the red BRITE magnitudes because their spectral window is cleaner than that of the blue magnitudes (see the insets in the lower panels of Fig. 1 ). We removed the orbital light-variation by pre-whitening with f orb , 2 f orb , 3 f orb , 4 f orb , and 6 f orb , divided the data into two parts as described above, and computed amplitude spectra. The results are displayed in Fig. 6 . The top left-hand panel shows the amplitude spectrum of the complete data (referred to as set 1 in the caption to the figure) with the peaks at the frequencies appearing in equations ( 2 )– ( 5 ) labelled. The upper middle left-hand panel shows the amplitude spectrum of the magnitudes covering the orbital phases from the western to eastern quadrature, i.e. the phases from 0.3825 to 0.8825 in Figs 3 and 5 (set 2). The peak at f n ,0 = ( f 2 + f 4 )/2 = 0.4857 d −1 and its f orb aliases dominate the spectrum. The aliases occur at the same frequencies as the f 2 and f 4 peaks in the top left-hand panel but should not be confused with them. While the aliases reproduce the side-lobes of the spectral window seen in the top right-hand panel, the frequencies f 2 and f 4 arise as the result of a transformation of the corotating frame of reference whose polar axis coincides with the line joining the components’ mass centres to the non-rotating frame with the polar axis parallel to the pulsating component’s rotation axis (see the second paragraph of this section). The lower middle left-hand panel contains the amplitude spectrum obtained from the set 2 data pre-whitened with f n ,0 . Now, the highest peak appears at