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From the main sequence to their late evolutionary stages, massive stars spendmost of their life as hot stars. Due to their high effective temperatures, themaximum of their emitted flux falls into the ultraviolet (UV) regime.Consequently, these stars emit a significant number of photons with energiessufficiently high enough to ionize hydrogen and other elements. As simple asthese fundamental considerations are, as complex is a realistic estimate of theresulting ionizing fluxes, in particular for energies above 54 eV. Estimatingthe ionizing flux budget of hot stars requires accurate models of theirspectral energy distributions (SEDs), covering in particular the far andextreme UV region. Modern atmosphere models that incorporate the so-calledline-blanketing effect, i.e. taking into account the millions of lines fromiron and other elements, yield a complex picture, illustrating that the SED ofa hot, massive star usually deviates significantly from a blackbody.

Massive Stars in the Far and Extreme Ultraviolet