Notes. The true anomaly is the initial value, ṁ_w stands for the mass-loss rate. Additional wind parameters v_c and denote the terminal velocities of the assumed spherical wind from the centre and the star, respectively. In these examples we performed integration runs with 1000 numerical particles representing the material of an initially spherical cloud, whereas the circumbinary disc population consisted of 500 particles with semi-major axes uniformly distributed from 10 AU to 50 AU, inclinations up to 30°, and eccentricities ranging from 0.0 to 0.1. The spherical cloud population adopts a Gaussian distribution in the phase space with the initial FWHMs of 12.5 mas and 5 km s^-1. In both examples, the integration starts at the true anomaly of −167° for the barycentre position.