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Time-resolved spectroscopic observations of rapidly oscillating Ap (roAp)stars show a complex picture of propagating magneto-acoustic pulsation waves,with amplitude and phase strongly changing as a function of atmospheric height.We have recently conducted numerical, non-linear MHD simulations to get aninsight into the complex atmospheric dynamics of magnetic pulsators. Here weuse the resulting time-dependent atmospheric structure and velocity field topredict line profile variations for roAp stars. These calculations userealistic atmospheric structure, account for vertical chemical stratificationand treat the line formation in pulsating stellar atmosphere without relying onthe simplistic single-layer approximation universally adopted for non-radialpulsators. The new theoretical calculations provide an essential tool forinterpreting the puzzling complexity of the spectroscopic pulsations in roApstars.

Towards pulsation mode identification in 3-D: theoretical simulations of line profile variations in roAp stars