Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...242...93m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 242, no. 1, Feb. 1991, p. 93-111.
Astronomy and Astrophysics
Astrophysics
154
Active Galactic Nuclei, Metallicity, Star Formation Rate, Wolf-Rayet Stars, Stellar Evolution, Stellar Mass, Stellar Models
Scientific paper
The minimum mass for WR star formation and the lifetimes in the WNL, WNE, WCL, WCE, and WO phases are derived as a function of initial metallicity Z and mass using evolutionary models of massive stars. The theoretical number ratios WR/O, WC/WR, and WC/WN are all found to increase strongly with increasing Z. Comparisons between theoretical and observed number ratios in galaxies of various Z in the Local Group show a remarkable agreement which supports the idea of Maeder et al. (1980) that Z is responsible for the enormous differences of the WR populations in galaxies with active star formation. The relative numbers of WN stars with and without hydrogen, identified with WNL and WNE stars respectively, are derived. The WNL phases generally last much longer for large initial masses, with little dependence on Z. The WNE phases are longer for lower initial masses and are shorter at Z = 0.04 than at Z = 0.02. The relative numbers of WC stars with various subtypes are also analyzed quantitatively.
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