Abstract
We show that the level of turbulence in accretion disks can be derived from a self-consistency requirement that the associated effective viscosity should match the instantaneous accretion rate. When turbulence originates in the magnetic shearing instability, the effective kinematic viscosity coefficient is shown to be describable by a Shakura-Sunyaev law with α ≈ 0.04. It is shown that thin disks supported by any turbulence with injection scale of order of the disk thickness, are very low magnetic Reynolds number systems. Turbulent viscosity-driven solutions with negligible field dragging and no emission of cold winds or jets are natural consequences of such regimes. Such disks are shown to expell the magnetic field of the accreting object from their kleplerian regions radially outwards, resulting in a flux distribution in the disk which differs very much from a dipolar one.
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© 1996 Kluwer Academic Publishers
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Heyvaerts, J.F., Bardou, A., Priest, E.R. (1996). Interaction of Turbulent Accretion Disks with Embedded Magnetic Fields. In: Tsinganos, K.C. (eds) Solar and Astrophysical Magnetohydrodynamic Flows. NATO ASI Series, vol 481. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0265-7_28
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DOI: https://doi.org/10.1007/978-94-009-0265-7_28
Publisher Name: Springer, Dordrecht
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