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تسجيل مستخدم جديدHelium and Nitrogen Enrichment in Massive Main Sequence Stars: Mechanisms and Implications for the Origin of WNL Stars
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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, $v , / , v_{rm crit} = 0$ to $0.6$, metallicity, $[mathrm{Fe}/mathrm{H}] = -4$ to $0$, and $alpha$-element enhancement, $[alpha/mathrm{Fe}] = 0$ 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 stars 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.
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