Abstract
Three body approximation is used to describe the rotational motion of the outer parts of the disk and the motion of the stream coming from the secondary component. The family of models, resulting from the numerical calculations, depends on two parameters: the mass-ratio and the dimension of the disk. The radial velocity data, when interpreted within this approximation, lead to: m1 = 0.9 m ⊙, m2 = 0.35 m ⊙, A = 1.0 x 1011 cm, R2 = 0.4 R⊙, and the radius-vector of the hot spot rs = 0.36A, with uncertainties up to 10–30 percent.
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© 1977 D. Reidel Publishing Company, Dordrecht, Holland
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Smak, J. (1977). Model of U Geminorum. In: Friedjung, M. (eds) Novae and Related Stars. Astrophysics and Space Science Library, vol 65. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-1217-1_10
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DOI: https://doi.org/10.1007/978-94-010-1217-1_10
Publisher Name: Springer, Dordrecht
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