3D view of the magnetised stellar wind for Models I and II. The surface magnetic field from March-June 2016 reconstructed by Bellotti et al. (2023) is used at the boundary of the models. The grey streamlines are the magnetic field lines embedded in the wind. The rotation axis of the star is along the z_⋆-axis. The 2D cut is placed at the x_⋆z_⋆ plane, and for reference the orbital distance of the planet is shown with the translucent sphere at 14.56 R_⋆ ≃ 0.028 au. The contour shows the wind velocity, and the Alfvén surface is shown by the translucent outer surface. Models I and II predict stellar wind mass-loss rates of 1.1 × 10⁻¹⁵ M_⊙ yr⁻¹ and 2.5 × 10⁻¹⁴ M_⊙ yr⁻¹.