In a 3D MHD simulation, the near-core magnetic field at the convective-radiative boundary is toroidally dominated and the rotational shear layer is confined to the Brunt-Väisälä peak, contradicting the dipolar assumption in magneto-asteroseismology.
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On the Geometry of the Near-Core Magnetic Field in Massive Stars
In a 3D MHD simulation, the near-core magnetic field at the convective-radiative boundary is toroidally dominated and the rotational shear layer is confined to the Brunt-Väisälä peak, contradicting the dipolar assumption in magneto-asteroseismology.