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Stellar Evolution in the Early Universe

Published online by Cambridge University Press:  01 June 2008

Raphael Hirschi ,
Urs Frischknecht ,
F.-K. Thielemann ,
Marco Pignatari ,
Cristina Chiappini ,
Sylvia Ekström ,
Georges Meynet  and
André Maeder
Raphael Hirschi
Affiliation:
Astrophysics group, Keele University, Lennard-Jones Lab., Keele, ST5 5BG, UK email: r.hirschi@epsam.keele.ac.uk IPMU, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
Urs Frischknecht
Affiliation:
Dept. of Physics & Astronomy, University of Basel, CH-4056, Basel, Switzerland
F.-K. Thielemann
Affiliation:
Dept. of Physics & Astronomy, University of Basel, CH-4056, Basel, Switzerland
Marco Pignatari
Affiliation:
Astrophysics group, Keele University, Lennard-Jones Lab., Keele, ST5 5BG, UK email: r.hirschi@epsam.keele.ac.uk JINA, University of Notre Dame, Notre Dame, IN 46556, USA
Cristina Chiappini
Affiliation:
Observatoire Astronomique de l'Université de Genève, CH-1290, Sauverny, Switzerland Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34131 Trieste, Italia
Sylvia Ekström
Affiliation:
Observatoire Astronomique de l'Université de Genève, CH-1290, Sauverny, Switzerland
Georges Meynet
Affiliation:
Observatoire Astronomique de l'Université de Genève, CH-1290, Sauverny, Switzerland
André Maeder
Affiliation:
Observatoire Astronomique de l'Université de Genève, CH-1290, Sauverny, Switzerland
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Abstract

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Massive stars played a key role in the early evolution of the Universe. They formed with the first halos and started the re-ionisation. It is therefore very important to understand their evolution. In this paper, we describe the strong impact of rotation induced mixing and mass loss at very low metallicity (Z). The strong mixing leads to a significant production of primary 14N, 13C and 22Ne. Mass loss during the red supergiant stage allows the production of Wolf-Rayet stars, type Ib,c supernovae and possibly gamma-ray bursts (GRBs) down to almost Z = 0 for stars more massive than 60 M⊙. Galactic chemical evolution models calculated with models of rotating stars better reproduce the early evolution of N/O, C/O and 12C/13C. We calculated the weak s-process production induced by the primary 22Ne and obtain overproduction factors (relative to the initial composition, Z = 10−6) between 100-1000 in the mass range 60–90 M⊙.

Keywords

Stars: mass lossstars: Population IIstars: rotationstars: supernovaestars: Wolf-RayetGalaxy: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 297 - 304
Copyright
Copyright © International Astronomical Union 2008

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