Magnetic quenching of the inverse cascade in rapidly rotating convective turbulence

Abstract

We present results from an asymptotic magnetohydrodynamic model that is suited for studying the rapidly rotating, low viscosity regime typical of the electrically conducting fluid interiors of planets and stars. We show that the presence of sufficiently strong magnetic fields prevents the formation of large-scale vortices and saturates the inverse cascade at a finite length-scale. This saturation corresponds to an equilibrated state in which the energetics of the depth-averaged flows are characterized by a balance of convective power input and ohmic dissipation. A quantitative criteria delineating the transition between finite-size flows and domain-filling (large-scale) vortices in electrically conducting fluids is found. By making use of the inferred and observed properties of planetary interiors, our results suggest that convection-driven large-scale vortices do not form in the electrically conducting regions of many bodies.

arXiv commentSupplementary material included as ancillary file

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Cited by in corpus (5)

• Tidal dissipation due to the elliptical instability and turbulent viscosity in convection zones in rotating giant planets and stars
• Shape and size of large-scale vortices: A generic fluid pattern in geophysical fluid dynamics
• Asymptotic behaviour of rotating convection-driven dynamos in the plane layer geometry
• Effects of kinematic and magnetic boundary conditions on the dynamics of convection-driven plane layer dynamos
• Inverse cascade suppression and shear layer formation in MHD turbulence subject to a guide field and misaligned rotation