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Paper: Recurrent novae, classical novae, symbiotic novae, and population II novae
Volume: 261, The Physics of Cataclysmic Variables and Related Objects
Page: 595
Authors: Kato, M.
Abstract: Light curve analyses of the decay phase of nova outbursts are summarized. The nova duration is determined by the strong wind mass-loss which depends only on the white dwarf mass. Fast novae correspond to very massive white dwarfs and very slow novae correspond almost to the lower mass limit of white dwarfs. This relation is shown in both classical novae and recurrent novae. Light curves are theoretically reproduced for recurrent novae, U Sco, V394 CrA, CI Aql, V2487 Oph, RS Oph, T CrB, V745 Sco and V3890 Sgr, using a binary model composed of a white dwarf, an irradiated accretion disk, and a partly irradiated companion which is shadowed by the accretion disk. From the light curve fitting, we conclude that most of these objects contain a very massive white dwarf close to the Chandrasekhar mass limit (1.37 Modot for U Sco, V394 CrA T CrB and RS Oph, 1.35 Modot for V2487 Oph, V3890 Sgr and V745 Sco). They are strong candidates of type Ia SN progenitors. Population II novae have trends of slow evolution and small expanding velocity compared with disk novae.
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