Higgins, Erin R., Vink, Jorick S., Hirschi, Raphael et al. (2 more authors) (2023) Stellar wind yields of very massive stars. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. pp. 534-547. ISSN 0035-8711
Abstract
The most massive stars provide an essential source of recycled material for young clusters and galaxies. While very massive stars (VMSs, M>100) are relatively rare compared to O stars, they lose disproportionately large amounts of mass already from the onset of core H-burning. VMS have optically thick winds with elevated mass-loss rates in comparison to optically thin standard O-star winds. We compute wind yields and ejected masses on the main sequence, and we compare enhanced mass-loss rates to standard ones. We calculate solar metallicity wind yields from MESA stellar evolution models in the range 50-500, including a large nuclear network of 92 isotopes, investigating not only the CNO-cycle, but also the Ne-Na and Mg-Al cycles. VMS with enhanced winds eject 5-10 times more H-processed elements (N, Ne, Na, Al) on the main sequence in comparison to standard winds, with possible consequences for observed anticorrelations, such as C-N and Na-O, in globular clusters. We find that for VMS 95 per cent of the total wind yields is produced on the main sequence, while only ∼5 per cent is supplied by the post-main sequence. This implies that VMS with enhanced winds are the primary source of 26Al, contrasting previous works where classical Wolf-Rayet winds had been suggested to be responsible for galactic 26Al enrichment. Finally, 200 stars eject 100 times more of each heavy element in their winds than 50 stars, and even when weighted by an IMF their wind contribution is still an order of magnitude higher than that of 50 stars.
Metadata
Item Type: | Article |
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Authors/Creators: |
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Copyright, Publisher and Additional Information: | Funding Information: The authors acknowledge MESA authors and developers for their continued revisions and public accessibility of the code. JSV, AML, and ERH are supported by STFC funding under grant number ST/V000233/1 in the context of the BRIDGCE UK Network. RH acknowledges support from STFC, the World Premier International Research Centre Initiative (WPI Initiative), MEXT, Japan, and the IReNA AccelNet Network of Networks (National Science Foundation, Grant No. OISE-1927130). This article is based upon work from the ChETEC COST Action (CA16117) and the European Union’s Horizon 2020 research and innovation programme (ChETEC-INFRA, Grant No. 101008324). Publisher Copyright: © 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. |
Keywords: | nuclear reactions, nucleosynthesis, abundances,stars: abundances,stars: evolution,stars: interiors,stars: mass-loss,stars: massive |
Dates: |
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Institution: | The University of York |
Academic Units: | The University of York > Faculty of Sciences (York) > Physics (York) The University of York > Faculty of Sciences (York) |
Funding Information: | Funder Grant number SCIENCE AND TECHNOLOGY FACILITIES COUNCIL (STFC) ST/V000535/1 |
Depositing User: | Pure (York) |
Date Deposited: | 16 Jan 2024 18:30 |
Last Modified: | 25 Dec 2024 00:29 |
Published Version: | https://doi.org/10.1093/mnras/stad2537 |
Status: | Published |
Refereed: | Yes |
Identification Number: | 10.1093/mnras/stad2537 |
Related URLs: | |
Open Archives Initiative ID (OAI ID): | oai:eprints.whiterose.ac.uk:207609 |