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Modes and instabilities in magnetized spherical Couette flow

Published online by Cambridge University Press:  25 January 2013

A. Figueroa ,
N. Schaeffer ,
H.-C. Nataf  and
D. Schmitt
A. Figueroa
Affiliation:
ISTerre, Université de Grenoble 1, CNRS, F-38041 Grenoble, France
N. Schaeffer
Affiliation:
ISTerre, Université de Grenoble 1, CNRS, F-38041 Grenoble, France
H.-C. Nataf*
Affiliation:
ISTerre, Université de Grenoble 1, CNRS, F-38041 Grenoble, France
D. Schmitt
Affiliation:
ISTerre, Université de Grenoble 1, CNRS, F-38041 Grenoble, France
*
†Email address for correspondence: [email protected]
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Abstract

Several teams have reported peculiar frequency spectra for flows in a spherical shell. To address their origin, we perform numerical simulations of the spherical Couette flow in a dipolar magnetic field, in the configuration of the $DTS$ experiment. The frequency spectra computed from time-series of the induced magnetic field display similar bumpy spectra, where each bump corresponds to a given azimuthal mode number $m$. The bumps appear at moderate Reynolds number (${\simeq }2600$) if the time-series are long enough (${\gt }300$ rotations of the inner sphere). We present a new method that permits retrieval of the dominant frequencies for individual mode numbers $m$, and extraction of the modal structure of the full nonlinear flow. The maps of the energy of the fluctuations and the spatio-temporal evolution of the velocity field suggest that fluctuations originate in the outer boundary layer. The threshold of instability is found at ${\mathit{Re}}_{c} = 1860$. The fluctuations result from two coupled instabilities: high-latitude Bödewadt-type boundary layer instability, and secondary non-axisymmetric instability of a centripetal jet forming at the equator of the outer sphere. We explore the variation of the magnetic and kinetic energies with the input parameters, and show that a modified Elsasser number controls their evolution. We can thus compare with experimental determinations of these energies and find a good agreement. Because of the dipolar nature of the imposed magnetic field, the energy of magnetic fluctuations is much larger near the inner sphere, but their origin lies in velocity fluctuations that are initiated in the outer boundary layer.

JFM classification

Boundary Layers: Boundary layer stability Geophysical and Geological Flows: Geodynamo MHD and Electrohydrodynamics: MHD turbulence
Type
Papers
Information
Journal of Fluid Mechanics , Volume 716 , 10 February 2013 , pp. 445 - 469
Copyright
©2013 Cambridge University Press

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Footnotes

‡

Current address: Facultad de Ciencias, Universidad Autónoma del Estado de Morelos, 62209, Cuernavaca Morelos, México.

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Figueroa et al. supplementary movie

Map view of the time evolution of the azimuthal velocity uφ beneath the surface of the outer sphere (r = 0.95) in the reference numerical simulation (Pm = 10-3, Re = 2 611 and Λ = 3.4 _ 10-2). At the origin time, the fluid is at rest and the rotation rate of the inner sphere is set to f. Time t is measured in rotation periods of the inner sphere. There are 6 frames per turn and the movie lasts 100 turns. Note that the first instabilities appear at the equator and are axisymmetric. After about 24 turns, nonaxisymmetric instabilities show up.

Download Figueroa et al. supplementary movie(Video)
Video 18 MB

Figueroa et al. supplementary movie

Time evolution of the angular velocity ω = uφ/s in a meridional plane (φ = 0) for the same simulation as in movie 1.

Download Figueroa et al. supplementary movie(Video)
Video 13.8 MB