Chemical Abundances and Yields from Massive Stars

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dc.creatorMaeder, André
dc.creatorMeynet, Georges
dc.creatorHirschi, Raphael
dc.date2004-09-22
dc.date.accessioned2026-07-07T02:14:42Z
dc.date.available2026-07-07T02:14:42Z
dc.descriptionStellar rotation produces an internal mixing of the elements due to shear instability and meridional circulation. This leads to observable $N/C$ enhancements in massive stars above about 7--9 $M_{\odot}$. Rotation also favours mass loss by stellar winds. Mass loss effects dominate for masses above 30 $M_{\odot}$, while mixing dominates below that limit. The effects of mixing are also much larger at lower metallicity $Z$, because the internal $Ω$--gradients are steeper. This appears to be in agreement with observations in the SMC. At very low $Z$ and Z=0, mixing between the He--burning core and the H--burning shell leads to the production of primary N in intermediate mass stars. Such enrichments increase the metallicity of the rotating star, also massive Z=0 stars with moderate initial velocities currently reach break--up velocity during a fraction of the MS phase. Both effects favour mass loss in Z=0 stars, which have ejecta with abundance anomalies very similar to those of C--rich very metal poor stars.
dc.description14 pages, 12 figures, in proceedings ``Cosmic Abundances'', F.N. Bash and T.G. Barnes (eds.), ASP Conf. Ser
dc.identifierhttps://arxiv.org/abs/astro-ph/0409528
dc.identifierhttp://arxiv.org/abs/astro-ph/0409528
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8221
dc.subjectAstrophysics
dc.titleChemical Abundances and Yields from Massive Stars
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