Fig. 1
Computed stellar SEDs (black lines) modified by homogeneous matter-bounded H II regions (nH = 10 cm-3) for different escape fractions (colored lines as labeled). For the sources we have chosen the main-sequence spectra from the hot star model grid by Weber et al. (2015). The chemical composition of the H II regions is assumed to be the same as that of the corresponding stellar atmospheres. Shown are the Eddington fluxes normalized to the stellar radius.
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