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Active Modes and Dynamical Balances in MRI Turbulence of Keplerian Disks with a Net Vertical Magnetic Field

Journal Article · · The Astrophysical Journal (Online)
 [1];  [2];  [3];  [4]
  1. Univ. of Texas, Austin, TX (United States); DOE/OSTI
  2. Niels Bohr International Academy, Copenhagen (Denmark); Helmholtz-Zentrum Dresden-Rossendorf (Germany); Ilia State Univ., Tbilisi (Georgia); Tbilisi State Univ., Tbilisi (Georgia)
  3. Univ. of Texas, Austin, TX (United States)
  4. Ilia State Univ., Tbilisi (Georgia); Tbilisi State Univ., Tbilisi (Georgia)
+ Show Author Affiliations
Her,e we studied dynamical balances in magnetorotational instability (MRI) turbulence with a net vertical field in the shearing box model of disks. Analyzing the turbulence dynamics in Fourier ($$\boldsymbol{k}$$-)space, we identified three types of active modes that define the turbulence characteristics. These modes have lengths similar to the box size, i.e., lie in the small wavenumber region in Fourier space labeled "the vital area" and are (i) the channel mode, uniform in the disk plane with the smallest vertical wavenumber; (ii) the zonal flow mode, azimuthally and vertically uniform with the smallest radial wavenumber; and (iii) the rest (parasitic) modes. The rest modes comprise those harmonics in the vital area whose energies reach more than 50% of the maximum spectral energy. The rest modes individually are not so significant compared to the channel and zonal flow modes; however, the combined action of their multitude is dominant over these two modes. These three mode types are governed by the interplay of the linear and nonlinear processes, leading to their interdependent dynamics. The linear processes consist of disk flow nonmodality modified classical MRI with a net vertical field. The main nonlinear process is the transfer of modes over wavevector angles in Fourier space—the transverse cascade. The channel mode exhibits episodic bursts supplied by linear MRI growth, while the nonlinear processes mostly oppose this, draining the channel energy and redistributing it to the rest modes. As for the zonal flow, it does not have a linear source and is fed by nonlinear interactions of the rest modes.
Research Organization:
Univ. of Texas, Austin, TX (United States)
Sponsoring Organization:
Marie Sklodowska-Curie Foundation; Shota Rustaveli National Science Foundation of Georgia; USDOE Office of Science (SC)
Grant/Contract Number:
FG02-04ER54742
OSTI ID:
1609572
Journal Information:
The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 2 Vol. 866; ISSN 1538-4357
Publisher:
Institute of Physics (IOP)Copyright Statement
Country of Publication:
United States
Language:
English

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Hydrodynamic stability and mode coupling in Keplerian flows: local strato-rotational analysis text January 2007
Aspect ratio dependence in magnetorotational instability shearing box simulations text January 2008
On Self-Sustained Dynamo Cycles in Accretion Discs text January 2008
Disk Winds Driven by Magnetorotational Instability and Dispersal of Proto-Planetary Disks text January 2008
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MRI channel flows and their parasites text January 2009
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Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
accretion
accretion disks
astronomy & astrophysics
dynamo
instabilities
magnetohydrodynamics (MHD)
turbulence