Simulated environment of HD 63433. Top: steady-state coronal magnetic field structure obtained from our ZDI-driven stellar wind model. Open magnetic field lines are truncated at two stellar radii, while the closed field lines are not truncated. The star is seen equator on at the rotational phase 0.35. The large-scale structure exhibits a mostly dipolar topology. The colours are the same as Fig. 7. Bottom: Alfvén surface and wind radial speed. The two-lobed Alfvén surface is characteristic for a dipole-dominated coronal magnetic field. The intersection of the Alfvén surface and the stellar equatorial plane is shown as a white curve, while the the planetary orbits are shown in orange, red, and pink. The orbital plane is colour-coded by the wind radial speed.