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Classical main-sequence chemically peculiar stars show light variability thatoriginates in surface abundance spots. In the spots, the flux redistributiondue to line (bound-bound) and bound-free transitions is modulated by stellarrotation and leads to light variability. White dwarfs and hot subdwarfs mayalso have surface abundance spots either owing to the elemental diffusion or asa result of accretion of debris. We model the light variability of typicalwhite dwarfs and hot subdwarfs that results from putative surface abundancespots. We show that the spots with radiatively supported iron overabundance maycause observable light variability of hot white dwarfs and subdwarfs. Accretionof debris material may lead to detectable light variability in warm whitedwarfs. We apply our model to the helium star HD 144941 and conclude that thespot model is able to explain most of observed light variations of this star.

Light variability of white dwarfs and subdwarfs due to surface abundance spots