The effect of diffusion of magnetic field on flow structure in close binaries

The developed numerical model takes into account the turbulent diffusion of the magnetic field that is determined by the magnetic reconnections and the electric currents dissipation in turbulent vortexes as well as by the magnetic flux tubes buoyancy. To define the influence of the turbulent dissipation of the magnetic field on the flow structure we used the model of the ideal MHD and that of MHD with non-zero turbulent diffusivity. It was found out that in both models the flow structure has the same qualitative features as in pure HD solution: (i) the magnetized accretion disk forms in the system; (ii) all previously discovered waves still exist in the disk: the shock wave (''hot line”) forming due to the interaction between the circumdisk halo and the stream from the inner Lagrangian point L1, two arms of the tidal shock, the spiral precessional wave, and the bow shock caused by the motion of the accretor and the disk through the circumbinary envelope. It was also shown that in both models the magnetic field in the disk is mainly toroidal, and the presence of the magnetic field leads to the formation of the magnetosphere and the funnel flow near the magnetic poles of the primary star. Besides, we discovered that taking into consideration the turbulent diffusion of the magnetic field leads to the drastic change of the plasma parameter β (from ∼10-3 in ideal MHD model to ∼10-1 for the model with turbulent dissipation) and as a consequence to the significant changes in the obtained MHD flows. As a result, the turbulent diffusion significantly increases the mass of the accretion disk, decreases its outer radius, height and characteristic density. Moreover, we came to the conclusion that the turbulent diffusion decreases the accretion rate (2.5-3 times) of the system that can drastically change the observational properties of the system.