期刊
ASTROPHYSICAL JOURNAL
卷 561, 期 2, 页码 L179-L182出版社
IOP PUBLISHING LTD
DOI: 10.1086/324763
关键词
accretion, accretion disks; diffusion; instabilities; MHD; turbulence
The nonlinear evolution and saturation mechanism of the magnetorotational instability (MRI) are investigated using three-dimensional resistive MHD simulations. A local shearing box is used for our numerical analysis, and the simulations begin with a purely vertical magnetic field. We find that the magnetic stress in the nonlinear stage of the MRI is strongly fluctuating. The time evolution shows the quasi-periodic recurrence of spike-shaped variations, typically for a few orbits, which correspond to the rapid amplification of the magnetic field by the nonlinear growth of a two-channel solution followed by decay through magnetic reconnections. The increase rate of the total energy in the shearing box system is analytically related to the volume-averaged torque in the system. We find that at the saturated state this energy gain of the system is balanced with the increase of thermal energy, mostly due to joule heating. The spike-shaped time evolution is a general feature of the nonlinear evolution of the MRI in disks threaded by vertical fields and can be seen if the effective magnetic Reynolds number is larger than about unity.
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