Nonconservative Mass Transfer in Massive Binaries and the Formation of Wolf-Rayet+O Binaries

Abstract

The mass transfer efficiency during the evolution of massive binaries is still uncertain. We model the mass transfer processes in a grid of binaries to investigate the formation of Wolf-Rayet+O (WR+O) binaries, taking into account two kinds of non-conservative mass transfer models: Model I with rotation-dependent mass accretion and Model II of half mass accretion. Generally the mass transfer in Model I is more inefficient, with the average efficiency in a range of $\sim 0.2-0.7$ and $\lesssim 0.2$ for Case A and Case B mass transfer, respectively. We present the parameter distributions for the descendant WR+O binaries. By comparing the modeled stellar mass distribution with the observed Galactic WR+O binaries, we find that highly non-conservative mass transfer is required.

8 figures; accepted for publication in ApJ

References in corpus (9)

• Binary interaction dominates the evolution of massive stars
• Physical Properties of Wolf-Rayet Stars
• The effect of massive binaries on stellar populations and supernova progenitors
• The Galactic WN stars: Spectral analyses with line-blanketed model atmospheres versus stellar evolution models with and without rotation
• Toward Complete Statistics of Massive Binary Stars: Penultimate Results from the Cygnus OB2 Radial Velocity Survey
• The Galactic WC stars: Stellar parameters from spectral analyses indicate a new evolutionary sequence
• Efficiency of mass transfer in massive close binaries, Tests from double-lined eclipsing binaries in the SMC
• On the formation of Be stars through binary interaction
• Spatial distribution of Galactic Wolf-Rayet stars and implications for the global population

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