Astronomy and Astrophysics Mhd Instability in Differentially Rotating Cylindric Flows

The possibility that the magnetic shear-flow instability (MRI, Balbus-Hawley instability) might give rise to turbulence in a cylindric Couette flow is investigated through numerical simulations. The study is linear and the fluid flow is supposed to be incompressible and differentially rotating with a simple velocity profile with Ω = a + b/R 2. The simplicity of the model is counterbalanced by the fact that the study is fully global in all three spatial directions with boundaries on each side; finite diffusivities are also allowed. The investigation is also carried out for several values of the azimuthal wavenumber of the perturbations in order to analyse whether non-axisymmetric modes might be preferred, which might produce , in a non-linear extension of the study, a self-sustained magnetic field. We find that with magnetic field the instability is easier to be excited than without magnetic field. The critical Reynolds number for Pm= 1 is of order 50 independent of whether the nonmagnetic flow is stable or not. Also we find that i) the magnetic field strongly reduces the number of Taylor vortices, ii) the angular momentum is transported outwards and iii) for finite cylinders a netto dynamo-alpha effect results which is negative for the upper part of the cylinder and which is positive for the lower part of the cylinder. For magnetic Prandtl number smaller than unity the critical Reynolds number scales with Pm −0.65. If this was true even for very small magnetic Prandtl number (e.g. liquid sodium) the critical Reynolds number should reach the value 10 5 which is, however, also characteristic for nonlinear finite-amplitude hydrodynamic Taylor-Couette turbulence – so that we easily have to expect the simultaneous existence of both sorts of in-stabilities in cold accretion disks. Your thesaurus codes are: missing; you have not inserted them