Total Poynting flux as a function of the angle Θ between the background magnetic field B₀ and the incident plasma velocity v₀. The angle Θ is zero, when B₀ and v₀ are perpendicular (see Fig. 1). The Poynting flux is symmetric with respect to 90°. For the planetary bodies under consideration in this work, Θ falls into the range 0 ≤ Θ ≤ 180°. Note that in this figure, we additionally show the range − 90° ≤ Θ ≤ 0° for cases where such an orientation of the magnetic field and the velocity occur. The interaction strength and the Alfvén Mach number are chosen as and M_A = 0.04, M_A = 0.4 and M_A = 0.66, respectively. Solid lines are calculated with the full expression for the Poynting flux of Eq. (53) and dashed lines are calculated with the approximation of Eq. (55).