Dr Fiorenzo Vincenzo F.Vincenzo@hull.ac.uk
Lecturer in Astrophysics
Dr Fiorenzo Vincenzo F.Vincenzo@hull.ac.uk
Lecturer in Astrophysics
Todd A. Thompson
David H. Weinberg
Emily J. Griffith
James W. Johnson
Jennifer A. Johnson
We test the hypothesis that the observed first-peak (Sr, Y, Zr) and second-peak (Ba) s-process elemental abundances in low-metallicity Milky Way stars, and the abundances of the elements Mo and Ru, can be explained by a pervasive r-process contribution originating in neutrino-driven winds from highly-magnetic and rapidly rotating proto-neutron stars (proto-NSs). We construct chemical evolution models that incorporate recent calculations of proto-NS yields in addition to contributions from AGB stars, Type Ia supernovae, and two alternative sets of yields for massive star winds and core-collapse supernovae. For non-rotating massive star yields from either set, models without proto-NS winds underpredict the observed s-process peak abundances by $0.3$-$1\,\text{dex}$ at low metallicity, and they severely underpredict Mo and Ru at all metallicities. Models incorporating wind yields from proto-NSs with spin periods $P \sim 2$-$5\,\text{ms}$ fit the observed trends for all these elements well. Alternatively, models omitting proto-NS winds but adopting yields of rapidly rotating massive stars, with $v_{\rm rot}$ between $150$ and $300\,\text{km}\,\text{s}^{-1}$, can explain the observed abundance levels reasonably well for $\text{[Fe/H]}<-2$. These models overpredict [Sr/Fe] and [Mo/Fe] at higher metallicities, but with a tuned dependence of $v_{\rm rot}$ on stellar metallicity they might achieve an acceptable fit at all [Fe/H]. If many proto-NSs are born with strong magnetic fields and short spin periods, then their neutrino-driven winds provide a natural source for Sr, Y, Zr, Mo, Ru, and Ba in low-metallicity stellar populations. Conversely, spherical winds from unmagnetized proto-NSs overproduce the observed Sr, Y, and Zr abundances by a large factor.
Vincenzo, F., A. Thompson, T., H. Weinberg, D., J. Griffith, E., W. Johnson, J., & A. Johnson, J. (2021). Nucleosynthesis signatures of neutrino-driven winds from proto-neutron stars: a perspective from chemical evolution models. Monthly notices of the Royal Astronomical Society, 508(3), 3499-3507. https://doi.org/10.1093/mnras/stab2828
Journal Article Type | Article |
---|---|
Acceptance Date | Sep 27, 2021 |
Online Publication Date | Oct 5, 2021 |
Publication Date | 2021-12 |
Deposit Date | Mar 12, 2022 |
Publicly Available Date | Mar 28, 2022 |
Journal | Monthly notices of the Royal Astronomical Society |
Print ISSN | 0035-8711 |
Publisher | Oxford University Press |
Peer Reviewed | Peer Reviewed |
Volume | 508 |
Issue | 3 |
Pages | 3499-3507 |
DOI | https://doi.org/10.1093/mnras/stab2828 |
Keywords | Astrophysics of Galaxies; High Energy Astrophysical Phenomena; Solar and Stellar Astrophysics |
Public URL | https://hull-repository.worktribe.com/output/3946222 |
Published article
(1.9 Mb)
PDF
Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2021 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
The distribution of [α/Fe] in the Milky Way disc
(2021)
Journal Article
Evolution of N/O ratios in galaxies from cosmological hydrodynamical simulations
(2018)
Journal Article
About Repository@Hull
Administrator e-mail: repository@hull.ac.uk
This application uses the following open-source libraries:
Apache License Version 2.0 (http://www.apache.org/licenses/)
Apache License Version 2.0 (http://www.apache.org/licenses/)
SIL OFL 1.1 (http://scripts.sil.org/OFL)
MIT License (http://opensource.org/licenses/mit-license.html)
CC BY 3.0 ( http://creativecommons.org/licenses/by/3.0/)
Powered by Worktribe © 2024
Advanced Search