FLiTs spectra of the disk models up to 0.32 Myr old, convolved to a spectral resolution R = 2800 (black lines) and R = 600 (red lines). Where indicated, the spectra were multiplied by 5, 10, or 50 to improve visibility. This disk is at an inclination of 45°. The reason why the spectral lines become weaker at 0.032 Myr, only to become stronger again at 0.056 Myr, is likelydue to the dust evolution; Fig. 1 shows that radii smaller than 1 AU, the gas-to-dust ratio drops between the 0.018 and 0.032 Myr models, before increasing again at the 0.056 Myr mark. Because the onset of radial drift suddenly decreases the gas-to-dust ratio, we see a corresponding drop in line fluxes.