The solar tachocline is the rotational transition near the base of the convection zone, approximately at solar radii, between differential rotation above and more nearly uniform rotation in the radiative interior. Its shear can contribute to the Omega effect, and stable stratification can help store strong toroidal magnetic fields. It is a proposed site for important parts of the solar dynamo, rather than a demonstrated unique location for all field generation.
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The tachocline is a region in the Sun's interior that separates the radiative zone from the convective zone. It is found approximately between 0.7 and 0.9 solar radii from the center of the Sun. In this layer, the rotational dynamics of the Sun undergo a significant transition. In the radiative zone, energy is transported outward by radiation, and the material rotates uniformly.