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Grids of stellar models with rotation VII: models from 0.8 to 300 M-circle dot at supersolar metallicity (Z=0.020)

Yusof, Norhasliza; Hirschi, Raphael; Eggenberger, Patrick; Ekström, Sylvia; Georgy, Cyril; Sibony, Yves; Crowther, Paul A; Meynet, Georges; Abu Kassim, Hasan; Aishah Wan Harun, Wan; Maeder, André; Groh, Jose H; Farrell, Eoin; Murphy, Laura

Grids of stellar models with rotation VII: models from 0.8 to 300 M-circle dot at supersolar metallicity (Z=0.020) Thumbnail


Authors

Norhasliza Yusof

Patrick Eggenberger

Sylvia Ekström

Cyril Georgy

Yves Sibony

Paul A Crowther

Georges Meynet

Hasan Abu Kassim

Wan Aishah Wan Harun

André Maeder

Jose H Groh

Eoin Farrell

Laura Murphy



Abstract

We present a grid of stellar models at supersolar metallicity (Z = 0.020) extending the previous grids of Geneva models at solar and sub-solar metallicities. A metallicity of Z = 0.020 was chosen to match that of the inner Galactic disc. A modest increase of 43 per?cent (= 0.02/0.014) in metallicity compared to solar models means that the models evolve similarly to solar models but with slightly larger mass-loss. Mass-loss limits the final total masses of the supersolar models to 35?M? even for stars with initial masses much larger than 100?M?. Mass-loss is strong enough in stars above 20?M? for rotating stars (25?M? for non-rotating stars) to remove the entire hydrogen-rich envelope. Our models thus predict SNII below 20?M? for rotating stars (25?M? for non-rotating stars) and SNIb (possibly SNIc) above that. We computed both isochrones and synthetic clusters to compare our supersolar models to the Westerlund 1 (Wd1) massive young cluster. A synthetic cluster combining rotating and non-rotating models with an age spread between log10(age/yr) = 6.7 and 7.0 is able to reproduce qualitatively the observed populations of WR, RSG, and YSG stars in Wd1, in particular their simultaneous presence at log10(L/L?) = 5–5.5. The quantitative agreement is imperfect and we discuss the likely causes: synthetic cluster parameters, binary interactions, mass-loss and their related uncertainties. In particular, mass-loss in the cool part of the HRD plays a key role.

Journal Article Type Article
Acceptance Date Jan 20, 2022
Online Publication Date Jan 31, 2022
Publication Date Feb 15, 2022
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 511
Issue 2
Pages 2814 - 2828
DOI https://doi.org/10.1093/mnras/stac230
Keywords stars: evolution; massive; rotation
Publisher URL https://academic.oup.com/mnras/article-abstract/511/2/2814/6517701?redirectedFrom=fulltext

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