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A model of magnetic braking of solar rotation

In the presence of differential rotation, a seed poloidal magnetic field can be wound up into a strong toroidal field. In this case, the azimuthal component of the magnetic tension term of the Lorentz force can break the original differential rotation. We use comsol to solve the corresponding MHD equations in a 2D geometry and show that under certain circumstances this mechanism can explain the rotational braking of solar-type stars.