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The purpose of this work was to obtain diffusion coefficient for the magneticangular momentum transport and material transport in a rotating solar model. Weassumed that the transport of both angular momentum and chemical elementscaused by magnetic fields could be treated as a diffusion process. Thediffusion coefficient depends on the stellar radius, angular velocity, and theconfiguration of magnetic fields. By using of this coefficient, it is foundthat our model becomes more consistent with the helioseismic results of totalangular momentum, angular momentum density, and the rotation rate in aradiative region than the one without magnetic fields. Not only can themagnetic fields redistribute angular momentum efficiently, but they can alsostrengthen the coupling between the radiative and convective zones. As aresult, the sharp gradient of the rotation rate is reduced at the bottom of theconvective zone. The thickness of the layer of sharp radial change in therotation rate is about 0.036 $R_{\odot}$ in our model. Furthermore, thedifference of the sound-speed square between the seismic Sun and the model isimproved by mixing the material that is associated with angular momentumtransport.

Angular momentum transport and element mixing in the stellar interior I. Application to the rotating Sun