BAT99-9 -- a WC4 Wolf-Rayet star with nitrogen emission: Evidence for binary evolution?

Abstract

An analysis of the Large Magellanic Cloud (LMC) WC4 star BAT99-9 (HD 32125, FD 4, Brey 7, WS 3) shows that the star still contains photospheric nitrogen. Three N emission features (N V $\lambda \lambda 1238,1242$, N IV $\lambda 1719$, N IV $\lambda \lambda 3479-3485$) are unambiguously identified in the spectrum. CMFGEN models of the star yield a N/C ratio of $0.004\pm 0.002$ (by number) and a C/He ratio of $0.15_{-0.05}^{+0.10}$. Due to the similarity of BAT99-9 to other WC4 stars, and the good fit achieved by CMFGEN to both the classic WC4 spectrum, and the N lines, we argue that the N lines are intrinsic to BAT99-9. An examination of a limited set of rotating models for single star evolution at LMC and Galactic metallicities shows that a model with a Galactic metallicity ($z=0.014$) and a progenitor mass of around $50M_{\odot }$ can have a N/C ratio similar to, or larger than, what we observe for a significant fraction of its lifetime. However, the LMC models ($z=0.006$) are inconsistent with the observations. Both the single and binary BPASS models predict that many WC stars can have a N/C ratio similar to, or larger than, what we observe for a significant fraction of their lifetime. While the binary models cover a wider range of luminosities and provide a somewhat better match to BAT99-9, it is not currently possible to rule out BAT99-9 being formed through single star evolution, given the uncertainties in mass-loss rates, and the treatment of convection and mixing processes.

arXiv commentAccepted for publication in MNRAS

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