Detecting deep axisymmetric toroidal magnetic fields in stars - The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field

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Fig. 7.

Spectrum of the Laplace tidal equation in the non-magnetic (top) and magnetic (bottom) cases as a function of the radius for m = −1, ν = 10, and Ω = 22.19 Ω_⊙ using the 1.6 M_⊙γ Dor model at ZAMS. Blue (respectively, orange) dots correspond to modes with even (respectively, odd) Hough functions.

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