Jordan Schofield
Isotopic ratios for C, N, Si, Al, and Ti in C-rich presolar grains from massive stars
Schofield, Jordan; Pignatari, Marco; Stancliffe, Richard J.; Hoppe, Peter
Authors
Marco Pignatari
Richard J. Stancliffe
Peter Hoppe
Abstract
Certain types of silicon carbide (SiC) grains, e.g. SiC-X grains, and low density (LD) graphites are C-rich presolar grains that are thought to have condensed in the ejecta of core-collapse supernovae (CCSNe). In this work, we compare C, N, Al, Si, and Ti isotopic abundances measured in presolar grains with the predictions of 21 CCSN models. The impact of a range of SN explosion energies is considered, with the high energy models favouring the formation of a C/Si zone enriched in 12C, 28Si, and 44Ti. Eighteen of the 21 models have H ingested into the He-shell and different abundances of H remaining from such H-ingestion. CCSN models with intermediate to low energy (that do not develop a C/Si zone) cannot reproduce the 28Si and 44Ti isotopic abundances in grains without assuming mixing with O-rich CCSN ejecta. The most 28Si-rich grains are reproduced by energetic models when material from the C/Si zone is mixed with surrounding C-rich material, and the observed trends of the 44Ti/48Ti and 49Ti/48Ti ratios are consistent with the C-rich C/Si zone. For the models with H-ingestion, high and intermediate explosion energies allow the production of enough 26Al to reproduce the 26Al/27Al measurements of most SiC-X and LD graphites. In both cases, the highest 26Al/27Al ratio is obtained with H still present at XH ≈ 0.0024 in He-shell material when the SN shock is passing. The existence of H in the former convective He-shell points to late H-ingestion events in the last days before massive stars explode as a supernova.
Citation
Schofield, J., Pignatari, M., Stancliffe, R. J., & Hoppe, P. (2022). Isotopic ratios for C, N, Si, Al, and Ti in C-rich presolar grains from massive stars. Monthly notices of the Royal Astronomical Society, 517(2), 1803-1820. https://doi.org/10.1093/mnras/stac2498
Journal Article Type | Article |
---|---|
Acceptance Date | Aug 26, 2022 |
Online Publication Date | Oct 13, 2022 |
Publication Date | 2022-12 |
Deposit Date | Apr 28, 2023 |
Publicly Available Date | Apr 28, 2023 |
Journal | Monthly Notices of the Royal Astronomical Society |
Print ISSN | 0035-8711 |
Electronic ISSN | 1365-2966 |
Publisher | Oxford University Press |
Peer Reviewed | Peer Reviewed |
Volume | 517 |
Issue | 2 |
Pages | 1803-1820 |
DOI | https://doi.org/10.1093/mnras/stac2498 |
Public URL | https://hull-repository.worktribe.com/output/4176287 |
Files
Published paper
(2.8 Mb)
PDF
Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2022 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
You might also like
New Experimental 23Na(α, p)26Mg Reaction Rate for Massive Star and Type Ia Supernova Models
(2021)
Journal Article
Exploring the link between star and planet formation with Ariel
(2021)
Journal Article
A Large-scale Approach to Modeling Molecular Biosignatures: The Diatomics
(2022)
Journal Article
UVES analysis of red giants in the bulge globular cluster NGC 6522
(2021)
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 © 2024
Advanced Search