Pole-on view on the equatorial distribution of the kinetic power from wind-magnetospheric interaction (see text for details). The green (fast) and magenta (slow) velocity components of the stellar wind are identical as in Fig. 9 (top-left). The configuration of the exoplanet orbit (white ellipse), with respect to the structure of the stellar wind, maximises the radio power at P₁ (periastron), and yields a minimum in location P₂.