High-resolution toy model of a (k, m) = (0, 1) g-mode pulsation with a distorted amplitude in the secondary component of a close binary system, based on the parameter values of V456 Cyg, as listed in Table C.1. Top: Flux variability caused by the binary motion. Both stellar components are assumed to be spherical, leading to the absence of ellipsoidal variability in this model. Middle: Observed amplitude modulation as a function of the orbital phase. Bottom: Observed pulsation phase modulation as a function of the orbital phase, caused by the geometry of the pulsation amplitude distortion across the stellar surface.