Stellar Evolution with Rotation

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The VLT-FLAMES survey of massive stars: evolution of surface N abundances and effective temperature scales in the Galaxy and Magellanic Clouds (2007, methodology): “This has been discussed by Meynet & Maeder (2000), who showed that the surface nitrogen enrichments are more prnounced as the stellar mass is increased in their models.”
Effects of rotation on the evolution of primordial stars (2008, background): “As described in Meynet & Maeder (2000), the meridional circulation then establishes very quickly (1–2% of the MS time) an equilibrium profile of Ω(r) inside the star with the core spinning faster than the surface.”
Fast rotating massive stars and the origin of the abundance patterns in galactic globular clusters (2006, methodology): “…the massive star models in many respects (see Maeder & Meynet 2000, for references); in particular, rotating models can reproduce the chemical enrichment observed at the surface of OBA stars (Heger & Langer 2000; Meynet & Maeder 2000). to mass loss which is strongly enhanced in the rotating model.”
Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit (2008, background): “The latter is expected for very massive stars at the end of their main-sequence evolution and for fast rotators where fresh hydrogen is mixed into the stellar core (Meynet & Maeder 2000).”