Coriolis darkening in late-type stars - II. Effect of self-sustained magnetic fields in stratified convective envelopes

Open Access

Fig. 4.

Same as in Fig. 3, but for the equatorial dipole considered in Fig. 1b, with E = 3 × 10⁻⁵, Pr = 1, N_ρ = 3, Ra = 2.48 Ra_c, and Pm = 2. The relative contribution of the axial dipole alone (m = 0) for the cut-off degrees ℓ_cut = ℓ_max, denoted with $f_{dip}^{ax}$ $f_{\mathrm{dip}}^{\mathrm{ax}}$ , is also represented in green.

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