Abstract
The observational properties of recurrent novae are reviewed in this talk. The class of recurrent novae may be divided into subgroups as (a) systems with a dwarf secondary and (b) systems with a giant secondary. The primary in these systems is a white dwarf, accreting at rates ~ 10-8 M ⊙ yr-1. The outbursts are powered by thermonuclear runaway reactions on the surface of the white dwarf.
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Anupama, G.C. (1995). The General Trends of Recurrent Novae. In: Bianchini, A., Valle, M.D., Orio, M. (eds) Cataclysmic Variables. Astrophysics and Space Science Library, vol 205. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0335-0_6
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