Abstract
In this work a 3-D ‘Smoothed Particle Hydrodynamics’ ([1]; [4]; [5]) accretion disc is simulated where particles at its inner edge are dragged by a fast spinning compact central star, as in the case of the intermediate polars. The angular velocity of the central star is twice the orbital angular velocity w 0. This drag can be attributed mainly to viscous interaction in the dense compact star atmosphere, although magnetic coupling may also play a role.
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© 1996 Kluwer Academic Publishers
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Lanzafame, G., Belvedere, G., Molteni, D. (1996). Inner Edge Drag by an Asynchronous Primary and Accretion Disc Structure In Close Binaries. In: Evans, A., Wood, J.H. (eds) Cataclysmic Variables and Related Objects. Astrophysics and Space Science Library, vol 208. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0325-8_35
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DOI: https://doi.org/10.1007/978-94-009-0325-8_35
Publisher Name: Springer, Dordrecht
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