Magnetic field geometry, not just strength, reshapes tidal dissipation spectra in rotating convective envelopes, though frequency-averaged dissipation usually stays near the hydrodynamical prediction.
Axisymmetric shear Alfv \'e n modes of a spherical shell in a dipolar magnetic field
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Tidal dissipation in magnetised, rotating stars and planets: linear calculations exploring various magnetic field configurations
Magnetic field geometry, not just strength, reshapes tidal dissipation spectra in rotating convective envelopes, though frequency-averaged dissipation usually stays near the hydrodynamical prediction.