Helium and Nitrogen Enrichment in Massive Main Sequence Stars: Mechanisms and Implications for the Origin of WNL Stars

The evolutionary paths taken by massive stars with $M \gtrsim 60 , $\mathrm{M}$_\odot$ remain substantially uncertain. They begin their lives as main sequence (MS) O-stars. Depending on their masses, rotation rates, and metallicities, they can then encounter a wide range of evolutionary states with an equally broad set of possible surface compositions and spectral classifications. We present a new grid of calculations for the evolution of such stars that covers a broad range in mass, M/M${}_{\odot }=60$ to $150$, rotation rate, $v\mathrm{/}{v}_{\mathrm{c}\mathrm{r}\mathrm{i}\mathrm{t}}=0$ to $0.6$, metallicity, $[\mathrm{F}\mathrm{e}\mathrm{/}\mathrm{H}]=-4$ to $0$, and $\alpha$-element enhancement, $[\alpha \mathrm{/}\mathrm{F}\mathrm{e}]=0$ to $0.4$. We show that rotating stars undergo rotationally-induced dredge-up of nucleosynthetic products, mostly He and N, to their surfaces while still on the MS. Non-rotating metal-rich stars also reveal the products of nucleosynthesis on their surfaces because even modest amounts of mass loss expose their “fossil” convective cores: regions that are no longer convective, but which were part of the convective core at an early stage in the star’s evolution. Thus surface enhancement of He and N is expected for rotating stars at all metallicities, and for non-rotating stars if they are relatively metal-rich. We calculate a stellar atmosphere for a representative model from our grid, properly accounting for He- and N-enhancement, and show that the resulting spectrum provides a good match to observed WNL stars, strongly suggesting that the physical mechanisms we have identified are the ultimate cause of the WNL phase.