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Evolution of zero-metallicity massive stars

Published online by Cambridge University Press:  26 May 2016

Paola Marigo ,
Cesare Chiosi ,
Léo Girardi  and
Rolf-Peter Kudritzki
Paola Marigo
Affiliation:
Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, I-35122, Padova, Italia
Cesare Chiosi
Affiliation:
Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, I-35122, Padova, Italia
Léo Girardi
Affiliation:
Osservatorio Astronomico di Trieste, Via Tiepolo 11, I-34131, Trieste, Italia
Rolf-Peter Kudritzki
Affiliation:
Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, HI 96822, USA

Abstract

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We discuss the evolutionary properties of primordial massive and very massive stars, supposed to have formed from metal-free gas. Stellar models are presented over a large range of initial masses (8 M⊙ ≲ Mi ≲ 1000 M⊙), covering the hydrogen- and helium-burning phases up to the onset of carbon burning. In most cases the evolution is followed at constant mass. To estimate the possible effect of mass loss via stellar winds, recent analytic formalisms for the mass-loss rates are applied to the very massive models (Mi ≥ 120 M⊙).

Type
Part 2. Interiors of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 334 - 340
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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