Abstract
The viscosity in accretion disks derived from observations is many orders of magnitude larger than the molecular viscosity can account for. MHD turbulence may cause a drastic increase of effective viscosity. Using the cascade model we simulate magnetic turbulence in a differentially rotating disk. The magnetic field allows for an energy flow from small to larger length scales. The turbulent stress due to the combined action of turbulent velocity- and magnetic fields show large fluctuations around the mean. Bursts in the total turbulent energy are large contributors to the time averaged stress and thus to the effective viscosity. The simulations show that the shear force is sufficient to sustain the turbulence.
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