arXiv2005
We examine the role of rotation on the evolution and chemical yields of very metal--poor stars. The models include the same physics, which was applied successfully at the solar $Z$ and for the SMC, in particular, shear diffusion, meridional circulation, horizontal turbulence, and rotationally enhanced mass loss. Models of very low $Z$ experience a much stronger internal mixing in all phases than at solar $Z$. Also, rotating models at very low $Z$, contrary to the usual considerations, show a large mass loss, which mainly results from the efficient mixing of the products of the 3$α$ reaction into the H--burning shell. This mixing allows convective dredge--up to enrich the stellar surface in heavy elements during the red supergiant phase, which in turn favours a large loss of mass by stellar winds, especially as rotation also increases the duration of this phase. On the whole, the low $Z$ stars may lose about half of their mass. Massive stars initially rotating at half of their critical velocity are likely to avoid the pair--instability supernova. The chemical composition of the rotationally enhanced winds of very low $Z$ stars show large CNO enhancements by factors of $10^3$ to $10^7$, together with large excesses of $^{13}$C and $^{17}$O and moderate amounts of Na and Al. The excesses of primary N are particularly striking. When these ejecta from the rotationally enhanced winds are diluted with the supernova ejecta from the corresponding CO cores, we find [C/Fe], [N/Fe],[O/Fe] abundance ratios that are very similar to those observed in the C--rich, extremely metal--poor stars (CEMP). We show that rotating AGB stars and rotating massive stars have about the same effects on the CNO enhancements.