Abstract
The first massive stars triggered the onset of chemical evolution by releasing the first metals (elements heavier than helium) in the Universe. The nature of these stars and how the early chemical enrichment took place is still largely unknown. Rotational-induced mixing in the stellar interior can impact the nucleosynthesis during the stellar life of massive stars and lead to stellar ejecta having various chemical compositions. We present low and zero-metallicity 20, 25 and 40 M⊙ stellar models with various initial rotation rates and assumptions for the nuclear reactions rates. With increasing initial rotation, the yields of light (from ∼ C to Al) and trans-iron elements are boosted. The trans-iron elements (especially elements heavier than Ba) are significantly affected by the nuclear reaction uncertainties. The chemical composition of the observed CEMP (carbon-enhanced metal-poor) stars CS29528-028 and HE0336+0113 are consistent with the chemical composition of the material ejected by a fast rotating 40 M⊙ model.
Highlights
IntroductionThe nature of the short-lived first generations of massive stars, that released the first metals (elements heavier than helium) in the Universe, is still largely unknown (Nomoto et al 2013, Karlsson et al 2013)
The nature of the short-lived first generations of massive stars, that released the first metals in the Universe, is still largely unknown (Nomoto et al 2013, Karlsson et al 2013)
The ejecta composition of light and trans-iron elements is affected by rotation
Summary
The nature of the short-lived first generations of massive stars, that released the first metals (elements heavier than helium) in the Universe, is still largely unknown (Nomoto et al 2013, Karlsson et al 2013). The nature of these stars can be probed indirectly by investigating the origin of low-mass metal-poor stars observed in our neighborhood, some of which are almost as old as the Universe (Beers & Christlieb 2005, Frebel & Norris 2015). We discuss the possibility of the existence of fast rotating massive stars in the early Universe by confronting our model yields to the chemical composition of observed metal-poor stars
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
