Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...506l..57s&link_type=abstract
The Astrophysical Journal, Volume 506, Issue 1, pp. L57-L60.
Astronomy and Astrophysics
Astronomy
58
Accretion, Accretion Disks, Diffusion, Instabilities, Magnetohydrodynamics: Mhd, Turbulence
Scientific paper
The nonlinear saturation of the magnetorotational instability due to ohmic dissipation is investigated with two-dimensional magnetohydrodynamic simulations of accretion disks. We adopt a local disk model in which the physical quantities are assumed to be spatially uniform except for the shear velocity in the azimuthal direction. Starting with a weak vertical field, the magnetorotational instability is saturated in the nonlinear regime when the magnetic Reynolds number R_m is less than unity. In the saturated turbulent state, the growth of the magnetic field for the instability and the damping by the ohmic dissipation are almost balanced. The efficiency of angular momentum transport alpha is of the order of 10^-2 to 10^-3, and alpha is found to be inversely proportional to the initial beta value. When R_m>~1, channel solutions appear and the magnetic energy continues growing even with the dissipation process. We can roughly explain these features with the help of the results obtained by the linear analysis. Our conclusion is that the magnetic dissipation is one of the most important processes that determine the saturation level of the magnetorotational instability.
Inutsuka Shu-ichiro
Miyama Shoken M.
Sano Takayoshi
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