The abundances of carbon and nitrogen in the atmospheres of classical Be stars.

Implicit is an apparent trend that \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathrm{V_{turb}}$\end{document} V t u r b increases with \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$\mathrm{T_{eff}}$\end{document} T e f f .

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Since there does remain an overall trend of N enhancement at higher rotational velocity, there can still be a role for rotational mixing in predominately single star evolution, but it is becoming likely that binary evolution needs to be accounted for in order to explain the entire Hunter diagram.

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