Aims. We study the effect of rotation on sheared turbulence due to differential rotation in the solar tachocline. Methods. By solving quasi-linear equations for the fluctuating fields, we derive turbulence amplitude and turbulent transport coefficients (turbulent viscosity and diffusivity), taking into account the effects of shear and rotation on turbulence. We focus on the regions of the tachocline near the equator and the poles where rotation and shear are perpendicular and parallel, respectively. Results. For parameter values typical of the tachocline, we show that the shear reduces both turbulence amplitude and transport, more strongly in the radial direction (parallel to the shear) than in the horizontal one, resulting in anisotropic turbulence. Rotation further reduces turbulence amplitude and transport at the equator whereas it does not have much effect near the pole. The interaction between shear and rotation is shown to give rise to a novel non-diffusive flux of angular momentum (known as the Λ-effect), possibly offering a mechanism for the occurrence of a strong shear region in the solar interior. Further implications for the transport in the tachocline are discussed.
|Number of pages||4|
|Journal||Astronomy and Astrophysics|
|Publication status||Published - 1 Feb 2007|
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- Sun: rotation
- Turbulence sun: interior
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science