On the formation of WR + WR binaries

Details On the formation of WR + WR binaries On the formation of WR + WR binaries

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...249..411v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 249, no. 2, Sept. 1991, p. 411-416. Research supported by FNRS and EEC.

Astronomy and Astrophysics

Astrophysics

22

Binary Stars, Star Formation, Stellar Evolution, Wolf-Rayet Stars, Mass Transfer, Stellar Mass, Stellar Models, Stellar Winds

Scientific paper

The formation and observability of Wr + WR binaries is investigated, using Maeder's (1990) stellar evolution models, for primaries in the mass range 15 to 100 solar masses. Such binaries can only be formed for the largest masses in this range, and for a very narrow range of mass ratios close to 1. Due to severe constraints for the detection of such systems, they are not expected to be observed as spectroscopic or visual binaries. Moreover, those that might be observed are of the type WC + WC. Hence, all discovered WR stars of suspected type WN + WC are probably stars in a transition state.

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