Wolf-Rayet stars in clusters - The initial stellar masses and evolutionary connections between subtypes

Details Wolf-Rayet stars in clusters - The initial stellar masses and evolutionary connections between subtypes Wolf-Rayet stars in clusters - The initial stellar masses and evolutionary connections between subtypes

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...136..237s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 136, no. 2, July 1984, p. 237-242.

Astronomy and Astrophysics

Astrophysics

65

Star Clusters, Stellar Evolution, Stellar Mass, Stellar Spectra, Wolf-Rayet Stars, B Stars, O Stars, Open Clusters

Scientific paper

The membership of Wolf-Rayet stars in open clusters and OB associations is used to determine the initial mass Mi of stars becoming WR stars. A detailed discussion of the relation between the spectral types of the cluster turnoff and the initial mass of WR stars is made on the basis of stellar models. Lower limits 18 solar mass for WN stars and 35 solar mass for WC stars are obtained. From the study of WR stars in clusters and associations evolutionary connections are established between WR subtypes. The most massive stars (Mi greater than about 60 solar mass) evolve via WN7 into WC4-WC8 stars. In the mass range Mi = 35-60 solar mass an evolutionary sequence WN5, WN6 to WC8.5, WC9 to WO is found. From initial masses lower than 35 solar mass mainly WN3, WN4, and WN5 stars can be formed. Binary evolution appears to have a negligible effect on the lower limit of initial mass but introduces a systematic deviation into the evolutionary sequences mentioned above. Particularly, the WR subtypes formed by close binaries are generally earlier than those formed by single stars of the same initial mass.

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