Top: radial rms velocity as a function of normalized radius for five different models whose characteristics are summarized in Table 1. Bottom: amplitude of the most powerful peak in each model. We find that some waves in turb2 have sufficient amplitudes to go through the convective zone and emerge on the surface of the star (top boundary at 0.97 R_⊙). The hatched zone represents the values of surface solar g-modes predicted in the literature.