Yusof, Norhasliza and Hirschi, Raphael and Eggenberger, Patrick and Ekstrom, Sylvia and Georgy, Cyril and Sibony, Yves and Crowther, Paul A. and Meynet, Georges and Kassim, Hasan Abu and Harun, Wan Aishah Wan and Maeder, Andre and Groh, Jose H. and Farrell, Eoin and Murphy, Laura (2022) Grids of stellar models with rotation VII: models from 0.8 to 300 M-circle dot at supersolar metallicity (Z=0.020). Monthly Notices of the Royal Astronomical Society, 511 (2). pp. 2814-2828. ISSN 0035-8711, DOI https://doi.org/10.1093/mnras/stac230.
Full text not available from this repository.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-circle dot even for stars with initial masses much larger than 100 M-circle dot. Mass-loss is strong enough in stars above 20 K for rotating stars (25 M-circle dot for non-rotating stars) to remove the entire hydrogen-rich envelope. Our models thus predict SNII below 20 M-circle dot for rotating stars (25 M-circle dot 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 log(10)(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 log(10) (L/L-circle dot) = 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.
| Item Type: | Article |
|---|---|
| Funders: | Ministry of Education, Malaysia [FP042-2018A] [FP045-2021] |
| Uncontrolled Keywords: | Stars: Evolution; Stars: Massive; Stars: Rotation |
| Subjects: | Q Science > Q Science (General) Q Science > QC Physics |
| Divisions: | Faculty of Science > Department of Physics |
| Depositing User: | Ms. Juhaida Abd Rahim |
| Date Deposited: | 22 Aug 2022 06:56 |
| Last Modified: | 22 Aug 2022 06:56 |
| URI: | http://eprints.um.edu.my/id/eprint/33358 |
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