Flux density arising from star planet interaction as a function of stellar mass-loss rate (left and center) and the magnetic field of the planet (right). The emission expected from Saur–Turnpenney’s model is shown in orange, while the emission expected from Zarka-Lanza’s model is shown in blue. The overlap between both models is shown in brown. We show in pale red color the region when the planet is in the super-Alfvènic regime. The dashed black line represents an assumed detection threshold of 100 µJy. For the variation with respect to the magnetic field of the planet we used M = 1.92 Ṁ_⊙, which is the maximum value for the mass loss rate before entering the sub-Alfvènic regime. Left: expected flux density for an unmagnetized planet in a closed dipolar geometry, as a function of the stellar wind mass loss. The pale red colored region indicates the super-Alfvénic case, when our approach no longer applies. Center: the same as in the left panel, but for a magnetized planet with B_p = 2 G. Right: expected flux density for a closed dipolar geometry