Abstract
The synthetic equivalent width (W Hβ) of the line Hβ in emission is obtained for Hii regions opaque to the Lyman photon flux, with embedded OB associations with different initial chemical compositions and initial mass functions. The variation ofW Hβ as a function of the evolution of the ionizing stars is analysed. The observations ofW Hβ for M33, M101, and M51 by Searle (1971) are discussed.
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Dottori, H.A. The equivalent width of the Hβ emission line and the evolution of the Hii regions. Astrophys Space Sci 80, 267–280 (1981). https://doi.org/10.1007/BF00652928
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DOI: https://doi.org/10.1007/BF00652928