X-ray Emission Mechanisms in Accreting White Dwarfs

In this chapter, we consider the processes which can lead to X-ray emission from different types of cataclysmic variable stars (CVs). CVs are semidetached, binary star systems where material is transferred from the donor star (also known as the companion or secondary star) onto the white dwarf primary. CVs are divided into several subclasses based on the observed phenomenology in the optical and X-ray bands, which, in turn, is largely defined by the magnetic field strength of the accretor. In nonmagnetic systems, a variety of observed behaviors are identified, depending on the accretion rate: novae, dwarf novae, nova-like variables, symbiotic binaries, and super-soft sources are all examples of nonmagnetic CVs. In magnetic systems (polars and intermediate polars, or DQ Her and AM Her systems, respectively), the accretion flow is channeled to polar regions, and the observational appearance is different. X-rays are typically produced through hot or energetic processes, and in CVs they are formed via shocks (within a boundary layer or accretion column, or through interactions either internal to the nova ejecta or between the ejecta and a stellar wind) or from hydrogen burning (either steady fusion or a thermonuclear runaway). All of these different types of accreting white dwarfs are discussed here, considering both spectral and temporal variability in the different populations.