Spherical averages of luminosity (integrated radiative flux), radial velocity, and grain radius in the 1.5 M_⊙ model st28gm05n033, as a function of radial distance and time. In the top and bottom panels, an isotherm with a temperature representative of silicate condensation is shown (1150 K) to demonstrate the interplay between variable radiative heating and the inner edges of dust layers. The red, orange, and green vertical bars indicate the instants selected for Figs. 3 and 6. The dark area in the lower part of the top panel represents the deep stellar interior, where most of the energy flux is transported by convection. The plots are similar to the corresponding ones in Fig 4. However, it is important to note the differing spatial and temporal axes, and the different range in grain radii.