A comparison of local simulations and reduced models of MRI-induced turbulence
arXiv:0904.3190 · doi:10.1111/j.1365-2966.2009.14798.x
Abstract
We run mean-field shearing-box numerical simulations with a temperature-dependent resistivity and compare them to a reduced dynamical model. Our simulations reveal the co-existence of two quasi-steady states, a `quiet' state and an `active' turbulent state, confirming the predictions of the reduced model. The initial conditions determine on which state the simulation ultimately settles. The active state is strongly influenced by the geometry of the computational box and the thermal properties of the gas. Cubic domains support permanent channel flows, bar-shaped domains exhibit eruptive behaviour, and horizontal slabs give rise to infrequent channels. Meanwhile, longer cooling time-scales lead to higher saturation amplitudes.
MNRAS accepted, 9 pages, 11 figures
References in corpus (9)
- MHD simulations of the magnetorotational instability in a shearing box with zero net flux. II. The effect of transport coefficients
- Impact of dimensionless numbers on the efficiency of MRI-induced turbulent transport
- MHD simulations of the magnetorotational instability in a shearing box with zero net flux. I. The issue of convergence
- Aspect ratio dependence in magnetorotational instability shearing box simulations
- MRI channel flows and their parasites
- Turbulent transport and its effect on the dead zone in protoplanetary discs
- Shearingbox-implementation for the central-upwind, constraint-transport MHD-code NIRVANA
- Exact shering box solutions of MHD flows with resistivity, viscosity and cooling
- Long-term Nonlinear Behaviour of the Magnetorotational Instability in a Localised Model of an Accretion Disc
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- Parametric Survey of Nonaxisymmetric Accretion Disk Instabilities: Magnetorotational Instability to Super-Alfvénic Rotational Instability
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