Two different views of the Eddington flux H_λ times the square of the radius r² as a function of wavelength and velocity, displayed from the inner boundary to a radius equivalent of 16 000 km s^-1, for a model with energy deposition. Compared with the energy-conserving atmosphere shown in Fig. 15, the change in the spectral distribution of the flux does not appear quite as dramatic, because the flux produced as a result of the energy deposited in the atmosphere from the radioactive decay is added gradually with the local spectral characteristics. Thus, the blocking effect in the UV is less prominent (upper panel), but the emission in the optical is similar to the model without energy deposition (lower panel).