Abstract
We present a new model for the Galactic population of close double white dwarfs. The model accounts for the suggestion of the avoidance of a substantial spiral-in during mass transfer between a giant and a main-sequence star of comparable mass and for detailed cooling models. It agrees well with the observations of the local sample of white dwarfs if the initial binary fraction is ~50% and an ad hoc assumption is made that white dwarfs with M ≲ 0.3 M⊙ cool faster than the models suggest. About 1000 white dwarfs with V ≲ 15 have to be surveyed for detection of a pair which has M 1 + M 2 ≳ M Ch and will merge within 10 Gyr.
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Yungelson, L.R., Nelemans, G., Portegies Zwart, S.F., Verbunt, F. (2001). The Population of Close Double White Dwarfs in the Galaxy. In: Vanbeveren, D. (eds) The Influence of Binaries on Stellar Population Studies. Astrophysics and Space Science Library, vol 264. Springer, Dordrecht. https://doi.org/10.1007/978-94-015-9723-4_25
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DOI: https://doi.org/10.1007/978-94-015-9723-4_25
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