  This is an overview of non-equilibrium aspects of the formation of solar
continua and lines affecting the contributions by magnetic network and plage to
spectrally resolved solar irradiance. After a brief summary of these
contributions and a compact refresher of solar spectrum formation, the emphasis
is on graphical exposition. Major obstacles for simulation-based irradiance
studies are how to cope with NLTE scattering in the violet and ultraviolet line
haze and how to cope with retarded hydrogen opacities in infrared and mm
radiation.
