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Paper: Is a Large Initial Binary Fraction Compatible with Observed WR Populations?
Volume: 367, Massive Stars in Interactive Binaries
Page: 421
Authors: Dray, L.; Tout, C.
Abstract: Wolf-Rayet (WR) stars have a binary fraction which appears observationally to be moderate and to change little with metallicity. However at solar metallicity their direct progenitors, the O stars, have a much higher binary fraction. One method of accounting for this discrepency is the formation of large numbers of single WR stars from a population with an initially high binary fraction. In this paper we examine how such a population might come about and present models investigating the characteristics of WR stars arising from a couple of the potential routes. Although single stars from systems unbound by supernovae are able to match the number ratios and binary fractions of WR subtypes, they do not seem to match well to the observed runaway population.
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