Zero net flux MRI-turbulence in disks $-$ sustenance scheme and magnetic Prandtl number dependence

Abstract

We investigate sustenance and dependence on magnetic Prandtl number ($\mathrm{Pm}$) for magnetorotational instability (MRI)-driven turbulence in astrophysical Keplerian disks with zero net magnetic flux using standard shearing box simulations. We focus on the turbulence dynamics in Fourier space, capturing specific/noncanonical anisotropy of nonlinear processes due to disk flow shear. This is a new type of nonlinear redistribution of modes over wavevector orientations in Fourier space -- the nonlinear transverse cascade -- which is generic to shear flows and fundamentally different from usual direct/inverse cascade. The zero flux MRI has no exponentially growing modes, so its growth is transient, or nonmodal. Turbulence self-sustenance is governed by constructive cooperation of the transient growth of MRI and the nonlinear transverse cascade. This cooperation takes place at small wavenumbers (on the flow size scales) referred to as the vital area in Fourier space. The direct cascade transfers mode energy from the vital area to larger wavenumbers. At large $\mathrm{Pm}$, the transverse cascade prevails over the direct one, keeping most of modes' energy contained in small wavenumbers. With decreasing $\mathrm{Pm}$, however, the action of the transverse cascade weakens and can no longer oppose the action of direct cascade which more efficiently transfers energy to higher wavenumbers, leading to increased resistive dissipation. This undermines the sustenance scheme, resulting in the turbulence decay. Thus, the decay of zero net flux MRI-turbulence with decreasing $\mathrm{Pm}$ is attributed to topological rearrangement of the nonlinear processes when the direct cascade begins to prevail over the transverse cascade.

26 pages, 16 figures, accepted for publication in the Astrophysical Journal

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Cited by in corpus (8)

• MRI-driven dynamo at very high magnetic Prandtl numbers
• MRI turbulence in accretion discs at large magnetic Prandtl numbers
• Simulating the magnetorotational instability on a moving mesh with the shearing box approximation
• MRI turbulence in vertically stratified accretion discs at large magnetic Prandtl numbers
• Convective, absolute and global azimuthal magnetorotational instabilities
• An effective model for magnetic field amplification by the magnetorotational and parasitic instabilities
• MRI-driven $\alpha \Omega$ dynamo at high Pm numbers
• Gravitoturbulent dynamo in global simulations of gaseous disks