Schematic view of the star. The convective plumes occur in the upper layers of the star and go deeper into the convective region. They grow by turbulent entrainment of matter at their edges and reach the top of the radiative zone. There, each of them, characterized by their angular position (θ_i,φ_i), releases a part of their kinetic energy and generate internal waves which can propagate towards the center. In our work, we suppose that there are no reflected waves propagating from the center to the radiative/convective interface.