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Grids of stellar models with rotation: V. Models from 1.7 to 120 Msun at zero metallicity

Murphy, Laura J; Groh, Jose H; Ekström, Sylvia; Meynet, Georges; Pezzotti, Camila; Georgy, Cyril; Choplin, Arthur; Eggenberger, Patrick; Farrell, Eoin; Haemmerlé, Lionel; Hirschi, Raphael; Maeder, André; Martinet, Sebastién

Grids of stellar models with rotation: V. Models from 1.7 to 120 Msun at zero metallicity Thumbnail


Laura J Murphy

Jose H Groh

Sylvia Ekström

Georges Meynet

Camila Pezzotti

Cyril Georgy

Arthur Choplin

Patrick Eggenberger

Eoin Farrell

Lionel Haemmerlé

André Maeder

Sebastién Martinet


Understanding the nature of the first stars is key to understanding the early universe. With new facilities such as JWST we may soon have the first observations of the earliest stellar populations, but to understand these observations we require detailed theoretical models. Here we compute a grid of stellar evolution models using the Geneva code with the aim to improve our understanding of the evolution of zero-metallicity stars, with particular interest in how rotation affects surface properties, interior structure, and metal enrichment. We produce a range of models of initial masses (Mini) from 1.7 Msun to 120 Msun, focusing on massive models of 9 Msun < Mini < 120 Msun. Our grid includes models with and without rotation, with rotating models having an initial velocity of 40% of the critical velocity. We find that rotation strongly impacts the evolution of the first stars, mainly through increased core size and stronger H-burning shells during core He-burning. Without radiative mass loss, angular momentum builds at the surface in rotating models, thus models of initial masses Mini > 60 Msun reach critical rotation on the main sequence and experience mass loss. We find that rotational mixing strongly affects metal enrichment, but does not always increase metal production as we see at higher metallicities. This is because rotation leads to an earlier CNO boost to the H shell during He-burning, which may hinder metal enrichment depending on initial mass and rotational velocity. Electronic tables of this new grid of Population III models are publicly available.

Journal Article Type Article
Acceptance Date Dec 4, 2020
Online Publication Date Dec 10, 2020
Publication Date 2021-02
Publicly Available Date May 30, 2023
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 501
Issue 2
Pages 2745-2763
Keywords stars: evolution, stars: massive, stars: Population III, stars: rotation
Publisher URL


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