Magnetic star with a bi-layer Alfvén frequency, ω_A, core in the core, ω_A, env in the envelope, and a bi-layer rotation rate, Ω_core in the core, Ω_env in the envelope. The cavity for m–g–i modes lies between r_a and r_b in the radiative zone. They become evanescent in the region [R_core; r_a] when the TARM is applied. Magneto-inertial modes propagate in the convective core below the location R_core.