Magnetic and rotational quenching of the effect
arXiv:1712.08045 · doi:10.1051/0004-6361/201732519
Abstract
Context: Differential rotation in stars is driven by turbulent transport of angular momentum. Aims: To measure and parametrize the non-diffusive contribution to turbulent stress, known as effect, and its quenching as a function of rotation and magnetic field. Methods: Simulations of homogeneous, anisotropically forced turbulence in fully periodic cubes are used to extract the turbulent Reynolds and Maxwell stresses. Magnetic fields are introduced by imposing a uniform large-scale field on the system. Turbulent transport coefficients pertaining to the effect are obtained by fitting. Results: The numerical results agree qualitatively with analytic ones at slow rotation and low Reynolds numbers. This entails that vertical (horizontal) transport is downward (equatorward). The existence of a significant meridional effect is confirmed. Large-scale vorticity generation is found at rapid rotation when the Reynolds number exceeds a threshold value. The effect is severely quenched by large-scale magnetic fields due to the tendency of the Reynolds and Maxwell stresses to cancel each other. Rotational (magnetic) quenching of occurs at more rapid rotation (at lower field strength) in simulations than in theory. Conclusions: The current results largely confirm the earlier theoretical results but they also offer new insights: the non-negligible meridional effect possibly plays a role in the maintenance of meridional circulation in stars and the appearance of large-scale vortices raises the question of their effect on the angular momentum transport in stars. The results regarding magnetic quenching are consistent with the strong decrease of differential rotation in recent semi-global simulations and highlight the importance of including magnetic effects in differential rotation models. (abridged)
14 pages, 9 figures, version accepted to Astron. Astrophys
References in corpus (26)
- Mean-field concept and direct numerical simulations of rotating magnetoconvection and the geodynamo
- Solar differential rotation and meridional flow: The role of a subadiabatic tachocline for the Taylor-Proudman balance
- Inverse cascade and symmetry breaking in rapidly-rotating Boussinesq convection
- Large-scale vortices in rapidly rotating Rayleigh-Bénard convection
- Scale dependence of alpha effect and turbulent diffusivity
- Magnetically controlled stellar differential rotation near the transition from solar to anti-solar profiles
- Minimal tau approximation and simulations of the alpha effect
- High-resolution calculation of the solar global convection with the reduced speed of sound technique: II. Near surface shear layer with the rotation
- Reynolds stress and heat flux in spherical shell convection
- Helioseismic Imaging of Fast Convective Flows Throughout the Near-Surface Shear Layer
- Nonlinear magnetic diffusivity and alpha tensors in helical turbulence
- Memory effects in turbulent transport
- The radial gradient of the near-surface shear layer of the Sun
- Solar dynamo models with alpha-effect and turbulent pumping from local 3D convection calculations
- Jets and large-scale vortices in rotating Rayleigh-Bénard convection
- Characterizing the feedback of magnetic field on the differential rotation of solar-like stars
- The supernova-regulated ISM. III. Generation of vorticity, helicity and mean flows
- Nonlinear regimes in mean-field full-sphere dynamo
- Lambda-effect from forced turbulence simulations
- Large-scale dynamos in rapidly rotating plane layer convection
- Double-Cell Type Solar Meridional Circulation Based on Mean-Field Hydrodynamic Model
- Angular momentum transport in convectively unstable shear flows
- The existence of the Lambda effect in the solar convection zone indicated by SDO observations
- Nonkinematic solar dynamo models with double-cell meridional circulation
- Solar-cycle variation of the rotational shear near the solar surface
- Effect of heat flux on differential rotation in turbulent convection
Cited by in corpus (15)
- On the Origin of Solar Torsional Oscillations and Extended Solar Cycle
- Star-in-a-box simulations of fully convective stars
- Effects of a subadiabatic layer on convection and dynamos in spherical wedge simulations
- Transition from anti-solar to solar-like differential rotation: Dependence on Prandtl number
- Post-dynamical inspiral phase of common envelope evolution: Binary orbit evolution and angular momentum transport
- Turbulent viscosity and effective magnetic Prandtl number from simulations of isotropically forced turbulence
- Solar dynamo cycle variations with a rotational period
- Antisolar differential rotation of slowly rotating cool stars
- Effects of small-scale dynamo and compressibility on the effect
- Anisotropic turbulent transport with horizontal shear in stellar radiative zones
- Small-scale and large-scale dynamos in global convection simulations of solar-like stars
- Angular momentum transport by magnetoconvection and the magnetic modulation of the solar differential rotation
- Generation of mean flows in rotating anisotropic turbulence: The case of solar near-surface shear layer
- Modelling differential rotation of red giants: the case of the evolved sun
- Non-diffusive angular momentum transport in rotating -pinches