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

Gogichaishvili, D.; Mamatsashvili, G.; Horton, W.; Chagelishvili, G.

doi:10.3847/1538-4357/aadbad

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

Journal Article · Mon Oct 22 00:00:00 EDT 2018 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aadbad· OSTI ID:1609572

Gogichaishvili, D. ^[1];

^[2]; Horton, W. ^[1]; Chagelishvili, G. ^[3]

Univ. of Texas, Austin, TX (United States)
Niels Bohr International Academy, Copenhagen (Denmark); Helmholtz-Zentrum Dresden-Rossendorf (Germany); Ilia State Univ., Tbilisi (Georgia); Tbilisi State Univ., Tbilisi (Georgia)
Ilia State Univ., Tbilisi (Georgia); Tbilisi State Univ., Tbilisi (Georgia)

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.

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Research Organization:: Univ. of Texas, Austin, TX (United States)

Sponsoring Organization:: USDOE Office of Science (SC); Marie Sklodowska-Curie Foundation; Shota Rustaveli National Science Foundation of Georgia

Grant/Contract Number:: FG02-04ER54742; 795158; FR17-107

OSTI ID:: 1609572

Journal Information:: The Astrophysical Journal (Online), Vol. 866, Issue 2; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 4 works

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Angular momentum transport and large eddy simulations in magnetorotational turbulence: the small Pm limit Meheut, H.; Fromang, S.; Lesur, G. arXiv https://doi.org/10.48550/arxiv.1505.05661	text	January 2015
Local and global aspects of the linear MRI in accretion disks Latter, Henrik N.; Fromang, Sebastien; Faure, Julien arXiv https://doi.org/10.48550/arxiv.1508.03012	text	January 2015
Resolution Dependence of Magnetorotational Turbulence in the Isothermal Stratified Shearing Box Ryan, Benjamin R.; Gammie, Charles F.; Fromang, Sebastien arXiv https://doi.org/10.48550/arxiv.1702.00777	text	January 2017
On hydrodynamic shear turbulence in Keplerian disks: via transient growth to bypass transition Chagelishvili, G. D.; Zahn, J. -P.; Tevzadze, A. G. arXiv https://doi.org/10.48550/arxiv.astro-ph/0302258	text	January 2003
The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs Pessah, Martin E.; Chan, Chi-kwan; Psaltis, Dimitrios arXiv https://doi.org/10.48550/arxiv.astro-ph/0603178	text	January 2006
Global MHD simulations of stratified and turbulent protoplanetary discs. I. Model properties Fromang, Sebastien; Nelson, Richard P. arXiv https://doi.org/10.48550/arxiv.astro-ph/0606729	text	January 2006
The Balbus-Hawley instability in weakly ionised discs Wardle, Mark arXiv https://doi.org/10.48550/arxiv.astro-ph/9809349	text	January 1998
A Local Model for Angular Momentum Transport in Accretion Disks Driven by the Magnetorotational Instability Pessah, Martin E.; Chan, Chi-kwan; Psaltis, Dimitrios arXiv https://doi.org/10.48550/arxiv.astro-ph/0610565	text	January 2006

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Turbulence and order in magnetized flowing plasmas Ebrahimi, Fatima; Blackman, Eric; Horton, Wendell arXiv https://doi.org/10.48550/arxiv.2011.09633	preprint	January 2020

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