Abstract
We have constructed a grid of models representing an H II region produced by an evolving starburst embedded in a gas cloud of the same metallicity. The models were produced with the spectral energy distribution from a stellar evolutionary synthesis code as input for a photoionization code that computes the emission-line strengths and equivalent widths. Stellar evolution was assumed to proceed according to the models of Maeder. The radiation field was computed using the Kurucz model atmospheres, supplemented by the expanding non-LTE atmospheres of Schmutz et al. for stellar evolutionary phases with strong winds, making a significant improvement over previous works using classical static, plane-parallel model atmospheres. Models for stellar interiors and atmospheres being still in a phase of continuous improvement, our population synthesis models reflect the state of the art in 1995.
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