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I will discuss some fundamental mathematical features of eigenoscillations of a magnetic star after deriving the basic equations. I will also discuss the wave propagation in a stratified plane atmosphere with magnetic fields as fundamental basics, and then describe how to solve global modes. Finally, it is stressed that the theoretical investigation of line profile variation beyond a single-surface approximation is necessary in order to compare the observations of roAp stars, of which the vertical wavelength of oscillation is as short as the thickness of the line-forming layer, with high time-resolution, high spectral resolution, and high signal-to-noise ratio.

Session3D: STARS − Effects of magnetic fields on stellar pulsation