The close binary systems with active accretion called cataclysmic variables contain a white dwarf that is heated by the mass transfer from the late type secondary star. These heating effects are best visible in the UVwith satellites like GALEX, FUSE, and HST, while some clues also emerge from optical spectra obtained through the SDSS. Modeling these light curves and spectral energy distributions determines the temperatures of the white dwarfs and of the hot spots created by the accretion. At high accretion rates, the accretion disk or column dominates the light, but at low accretion rates, the white dwarf is visible and may be directly studied. Recent results from studies of this type have determined that pulsating white dwarfs in accreting systems exist in a different instability strip than single pulsators and that highly magnetic white dwarfs still have hot spots even when the mass transfer stream has ended.
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Szkody, P. (2008). Modeling the Hot Components in Cataclysmic Variables: Info on the White Dwarf and Hot Disk from GALEX, FUSE, HST and SDSS. In: Short-Period Binary Stars: Observations, Analyses, and Results. Astrophysics and Space Science Library, vol 352. Springer, Dordrecht. https://doi.org/10.1007/978-1-4020-6544-6_7
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