Plots of density distribution (color scale, in particles cm⁻³) for sub-Alfvénic (top) and super-Alfvénic (bottom) cases of our PLUTO simulations. The green lines correspond to streamlines of the stellar wind velocity, and the red lines to magnetic field lines of the stellar wind and of the planet. In both cases, B_p = 0.32 G and the tilt of the planet is i = 0 deg, i.e., B_p is perpendicular to B_imf. In the sub-Alfvénic case, no bow shock is formed, and the resulting radio emission originates only from the reconnecting region of the exoplanet magnetosphere. In the super-Alfvénic case, a bow shock is formed. The radio emission originates both from the reconnecting region of the magnetosphere and from the bow shock (see Sec. 5). Movies of these simulations, from beginning to end, when a steady solution is reached, are available online.