Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ap%26ss.307..191s&link_type=abstract
Astrophysics and Space Science, Volume 307, Issue 1-3, pp. 191-195
Astronomy and Astrophysics
Astrophysics
7
Accretion Disks, Mhd, Turbulence
Scientific paper
MHD turbulence driven by magnetorotational instability (MRI) in accretion disks is investigated using the local shearing box calculations. The growth of many short-wavelength MRI modes, which are called “channel flows”, is found in the spatial distribution of the current density. These small channel flows can be regarded as a unit structure of MRI driven turbulence. Nonlinear evolution of the channel flow affects the saturation amplitude and time variability of the Maxwell stress. Exponential growth of a channel mode is stopped by the Kelvin-Helmholtz type instability which triggers the subsequent magnetic reconnection. The characteristics of the magnetic reconnection are consistent with the Sweet-Parker model. These studies of the nonlinear evolution of the channel flow are required to understand the saturation mechanism of the MRI.
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