Turbulence-driven angular momentum transport in modulated Kepler flows

Details Turbulence-driven angular momentum transport in modulated Kepler flows Turbulence-driven angular momentum transport in modulated Kepler flows

2001-06-28

arxiv.org/abs/astro-ph/0106524v1

Astronomy and Astrophysics

Astrophysics

9 pages, 9 figures, Astron. Nachr., in press

Scientific paper

10.1002/1521-3994(200107)322:3<1

The velocity fluctuations in a spherical shell arising from sinusoidal perturbations of a Keplerian shear flow with a free amplitude parameter \epsilon are studied numerically by means of fully 3D nonlinear simulations. The investigations are performed at high Reynolds numbers, i.e. 3000 < Re < 5000. We find Taylor-Proudman columns of large eddies parallel to the rotation axis for sufficiently strong perturbations. An instability sets in at critical amplitudes with \epsilon_crit \propto Re^-1. The whole flow turns out to be almost axisymmetric and nonturbulent exhibiting, however, a very rich radial and latitudinal structure. The Reynolds stress is positive in the entire computational domain, from its Gaussian radial profile a positive viscosity-alpha of about 10^-4 is derived. The kinetic energy of the turbulent state is dominated by the azimuthal component whereas the other components are smaller by two orders of magnitude. Our simulations reveal, however, that these structures disappear as soon as the perturbations are switched off. We did not find an ``effective'' perturbation whose amplitude is such that the disturbance is sustained for large times (cf. Dauchot & Daviaud 1995) which is due to the effective violation of the Rayleigh stability criterion. The fluctuations rapidly smooth the original profile towards to pure Kepler flow which, therefore, proves to be stable in that sense.

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