Comparison of observed UV flux (IUE, mean low spectral resolution spectrum) with flux from model atmospheres for solar iron abundance ε_Fe =  − 4.6 and for a model without iron (the abundance of helium and silicon is ε_He =  − 1.0, ε_Si =  − 4.3). The depression at 1550   Å is a clear signature of iron. Both model fluxes were multiplied by a constant factor to match the observed spectrum and convolved with a Gaussian filter with a dispersion of 1.3 Å. The LWP12335 spectrum and predicted near-UV fluxes are overplotted in the upper right.