Phenomenology of turbulent dynamo growth and saturation

Abstract

With a non local shell model of magnetohydrodynamic turbulence we investigate numerically the turbulent dynamo action for low and high magnetic Prandtl numbers ($Pm$). The results obtained in the kinematic regime and along the way to dynamo saturation are understood in terms of a phenomenological approach based on the local ($Pm\ll 1$) or non local ($Pm\gg 1$) nature of the energy transfers. In both cases the magnetic energy grows at small scale and saturates as an inverse `` cascade ''.

arXiv comment17 pages, 6 figures, submitted to ApJ

References in corpus (10)

• Simulations of small-scale turbulent dynamo
• An optimal shell model of turbulence
• Spectral energy dynamics in magnetohydrodynamic turbulence
• Inverse cascade in decaying 3D magnetohydrodynamic turbulence
• Numerical study of dynamo action at low magnetic Prandtl numbers
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• A model of nonlinear evolution and saturation of the turbulent MHD dynamo
• Is nonhelical hydromagnetic turbulence peaked at small scales?
• Multi-scale Hall-MHD turbulence in the solar wind
• Shell-models of RMHD turbulence and the heating of solar coronal loops

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• Saturation of the Turbulent Dynamo
• Scale interactions in magnetohydrodynamic turbulence
• A 3D Simulation of a Neutrino-Driven Supernova Explosion Aided By Convection and Magnetic Fields
• Dynamos at extreme magnetic Prandtl numbers: Insights from shell models
• Energy transfers in dynamos with small magnetic Prandtl numbers
• Transition from large-scale to small-scale dynamo
• Cascades and dissipation ratio in rotating MHD turbulence at low magnetic Prandtl number
• Energy transfers in shell models for MHD turbulence
• Homopolar oscillating-disc dynamo driven by parametric resonance
• Intermittent turbulent dynamo at very low and high magnetic Prandtl numbers