The structure of cool accretion disc in semidetached binaries

Details The structure of cool accretion disc in semidetached binaries The structure of cool accretion disc in semidetached binaries

2004-03-02

arxiv.org/abs/astro-ph/0403053v1

Astron.Rep. 48 (2004) 449-456; Astron.Zh. 81 (2004) 494-502

Astronomy and Astrophysics

Astrophysics

LaTeX, 16 pages, 8 figures, to be published in Astron. Zh

Scientific paper

10.1134/1.1767212

We present the results of qualitative consideration of possible changes occurring during the transition from the hot accretion disc to the cool one. We argue the possible existence of one more type of spiral density waves in the inner part of the disc where gasdynamical perturbations are negligible. The mechanism of formation of such a wave as well as its parameters are considered. We also present the results of 3D gasdynamical simulation of cool accretion discs. These results confirm the hypothesis of possible formation of the spiral wave of a new, "precessional" type in the inner regions of the disc. Possible observational manifestations of this wave are discussed.

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