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The IACOB project XIII. Helium enrichment in O-type stars as a tracer of past binary interaction
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abstract
There is increasing evidence that single-star evolutionary models are inadequate to reproduce all observational properties of massive stars. Binary interaction has emerged as a key factor in the evolution of a significant fraction of massive stars. In this study, we investigate the helium ($Y_{\mathrm He}$) and nitrogen ($\epsilon_{\mathrm N}$) surface abundances in a comprehensive sample of 180 Galactic O-type stars with projected rotational velocities $v\sin(i)\leq150{\mathrm km}\cdot{\mathrm s}^{-1}$. We found a subsample ($\sim20\%$ of the total, and $\sim80\%$ of the stars with $Y_{\mathrm He}\geq0.12$) with a $Y_{\mathrm He}$ and $\epsilon_{\mathrm N}$ combined pattern unexplainable by single-star evolution. We argue that the stars with anomalous surface abundance patterns are binary interaction products.
Forward citations
Cited by 2 Pith papers
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The IACOB project XIX. Revisiting massive-star evolution with empirical TAMS constraints: updated models, overshoot calibration, and the population of blue supergiants
Massive-star models require mass-dependent core overshoot (α_ov ≈ 0.18–0.45) to match the empirical TAMS, but still fail to explain the velocity dependence of the TAMS and the observed blue supergiant population.
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Unravelling Mass Transfer in Algols from Surface Abundances. I. Z Vulpeculae
Z Vul's donor star shows a C/N ratio of 2.14, lacking the deep carbon depletion expected after mass stripping, and the fitted models favor nearly conservative Case A mass transfer.
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