Top panel: grain temperature as a function of distance from the star. Lower panel: spectral energy distributions as a function of wavelength. Structure from model A3 during the maximum luminosity phase. The dark red curves show temperature and spectra from snapshots with core-mantel grains of 5% thickness. The light red curves show the results from fitting the core-mantel spectra with snapshots of the atmosphere where we set the lower limit for the grain temperature to 525 K.