Abstract
The dynamics of accretion flow in close binary stars is investigated via a numerical simulation of the accretion flow. The importance of the secondary’s tidal torque is discussed with respect to the radius of the accretion disc. It is found that the steady-state disc has a fixed radius, which is within the primary’s Roche lobe, a result which differs from that of Livio & Verbunt (1988).
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References
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Whitehurst, Robert, 1988a. Mon. Not. R. astr. Soc., 232, 55.
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© 1989 Kluwer Academic Publishers
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Whitehurst, R. (1989). Simulations of Accretion Flow in Close Binary Stars. In: Meyer, F., Duschl, W.J., Frank, J., Meyer-Hofmeister, E. (eds) Theory of Accretion Disks. NATO ASI Series, vol 290. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-1037-9_20
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DOI: https://doi.org/10.1007/978-94-009-1037-9_20
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-6958-8
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