S Jones
Remnants and ejecta of thermonuclear electron-capture supernovae: Constraining oxygen-neon deflagrations in high-density white dwarfs
Jones, S; Röpke, F K; Fryer, C; Ruiter, A J; Seitenzahl, I R; Nittler, L R; Ohlmann, S T; Reifarth, R; Pignatari, M; Belczynski, K
Authors
F K Röpke
C Fryer
A J Ruiter
I R Seitenzahl
L R Nittler
S T Ohlmann
R Reifarth
M Pignatari
K Belczynski
Abstract
The explosion mechanism of electron-capture supernovae (ECSNe) remains equivocal: it is not completely clear whether these events are implosions in which neutron stars are formed, or incomplete thermonuclear explosions that leave behind bound ONeFe white dwarf remnants. Furthermore, the frequency of occurrence of ECSNe is not known, though it has been estimated to be of the order of a few per cent of all core-collapse supernovae. We attempt to constrain the explosion mechanism (neutron-star-forming implosion or thermonuclear explosion) and the frequency of occurrence of ECSNe using nucleosynthesis simulations of the latter scenario, population synthesis, the solar abundance distribution, pre-solar meteoritic oxide grain isotopic ratio measurements and the white dwarf mass-radius relation. Tracer particles from 3d hydrodynamic simulations were post-processed with a large nuclear reaction network in order to determine the complete compositional state of the bound ONeFe remnant and the ejecta, and population synthesis simulations were performed in order to estimate the ECSN rate with respect to the CCSN rate. The 3d deflagration simulations drastically overproduce the neutron-rich isotopes 48 Ca, 50 Ti, 54 Cr , 60 Fe and several of the Zn isotopes relative to their solar abundances. Using the solar abundance distribution as our constraint, we place an upper limit on the frequency of thermonuclear ECSNe as 1−3 % the frequency at which core-collapse supernovae (FeCCSNe) occur. This is on par with or 1 dex lower than the estimates for ECSNe from single stars. The upper limit from the yields is also in relatively good agreement with the predictions from our population synthesis simulations. The 54 Cr/ 52 Cr and 50 Ti/ 48 Ti isotopic ratios in the ejecta are a near-perfect match with recent measurements of extreme pre-solar meteoritc oxide grains, and 53 Cr/ 52 Cr can also be matched if the ejecta condenses before mixing with the interstellar medium. The composition of the ejecta of our simulations implies that ECSNe, including accretion-induced collapse of oxygen-neon white dwarfs, could actually be partial thermonuclear explosions and not implosions that form neutron stars. There is still much work to do to improve the hydrodynamic simulations of such phenomena, but it is encouraging that our results are consistent with the predictions from stellar evolution modelling and population synthesis simulations, and can explain several key isotopic ratios in a subset of pre-solar oxide meteoritic grains. Theoretical mass-radius relations for the bound ONeFe WD remnants of these explosions are apparently consistent with several observational WD candidates. The composition of the remnants in our simulations can reproduce several, but not all, of the spectroscopically-determined elemental abundances from one such candidate WD.
Citation
Jones, S., Röpke, F. K., Fryer, C., Ruiter, A. J., Seitenzahl, I. R., Nittler, L. R., Ohlmann, S. T., Reifarth, R., Pignatari, M., & Belczynski, K. (2019). Remnants and ejecta of thermonuclear electron-capture supernovae: Constraining oxygen-neon deflagrations in high-density white dwarfs. Astronomy and Astrophysics, 622, Article A74. https://doi.org/10.1051/0004-6361/201834381
Journal Article Type | Article |
---|---|
Acceptance Date | Dec 13, 2018 |
Online Publication Date | Dec 21, 2018 |
Publication Date | Feb 1, 2019 |
Deposit Date | Jan 7, 2019 |
Publicly Available Date | Jan 8, 2019 |
Print ISSN | 0004-6361 |
Publisher | EDP Sciences |
Peer Reviewed | Peer Reviewed |
Volume | 622 |
Article Number | A74 |
DOI | https://doi.org/10.1051/0004-6361/201834381 |
Keywords | stars: evolution; stars: interiors; stars: neutron; supernovae: general |
Public URL | https://hull-repository.worktribe.com/output/1207696 |
Publisher URL | https://www.aanda.org/articles/aa/abs/2019/02/aa34381-18/aa34381-18.html |
Contract Date | Jan 8, 2019 |
Files
article with full citation details
(4.3 Mb)
PDF
Copyright Statement
Reproduced with permission from Astronomy & Astrophysics, © ESO
article
(3.2 Mb)
PDF
Copyright Statement
© ESO 2018
You might also like
Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
(2023)
Journal Article
The chemical evolution of the solar neighbourhood for planet-hosting stars
(2023)
Journal Article
Progress on nuclear reaction rates affecting the stellar production of <sup>26</sup>Al
(2023)
Journal Article
Downloadable Citations
About Repository@Hull
Administrator e-mail: repository@hull.ac.uk
This application uses the following open-source libraries:
SheetJS Community Edition
Apache License Version 2.0 (http://www.apache.org/licenses/)
PDF.js
Apache License Version 2.0 (http://www.apache.org/licenses/)
Font Awesome
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 © 2025
Advanced Search