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Paper: Precessional Density Wave as a Reason of Turbulence in Accretion Disks of Non-magnetic Close Binary Stars
Volume: 498, Numerical Modeling of Space Plasma Flows ASTRONUM-2014
Page: 41
Authors: Bisikalo, D. V.; Kurbatov, E. P.; Kaygorodov, P. V.
Abstract: 3D numerical simulations demonstrate the formation of precessional spiral density waves in accretion disks of close binary stars. The precesional wave occurs in the Keplerian disk as a result of gravitational action of the donor-star. The wave causes the appearance of strong density and velocity gradients in the disk. Linear stability analysis shows that the presence of a radial velocity gradient leads to the instability of radial modes. The perturbation becomes unstable if the radial velocity variations are of the same order or greater than the sound speed on the characteristic wave scale of the perturbations. The unstable perturbations rapidly grow with time and give rise to the emergence and growth of turbulence in the accretion disk. The obtained viscosity (0.01 in terms of Shakura-Sunyaev parameter) is in agreement with observations.
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