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Published online by Cambridge University Press: 05 April 2019
Any white dwarf or neutron star that accretes enough material from a red giant companion, such that this interaction can be detected at some wavelength, is currently termed asymbiotic star (orbital period ∼2–3 years). In the majority of ∼400 known systems, the white dwarf burns nuclearly at its surface the accreted material, and the resulting high temperatureand luminosity allow ionisation of a large fraction of the cool giant’s wind. X-ray observations are revealing the existence of a parallel (and large ?) population of optically quiet, accreting-only symbiotic stars. Accretion flows and disks, ionisation fronts and shock, complex 3D geometries and new evolution channels are gaining relevance and are reshaping our understanding of symbiotic stars. The chapter reviews the different types of symbiotic stars currently in the family and their variegated outburst behaviours.
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