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Hydrodynamic simulations of electron-capture supernovae: progenitor and dimension dependence

Zha, Shuai and O’Connor, Evan P. and Couch, Sean M. and Leung, Shing-Chi and Nomoto, Ken’ichi (2022) Hydrodynamic simulations of electron-capture supernovae: progenitor and dimension dependence. Monthly Notices of the Royal Astronomical Society, 513 (1). pp. 1317-1328. ISSN 0035-8711. doi:10.1093/mnras/stac1035. https://resolver.caltech.edu/CaltechAUTHORS:20220525-90854000

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Abstract

We present neutrino-transport hydrodynamic simulations of electron-capture supernovae (ECSNe) in flash with new two-dimensional (2D) collapsing progenitor models. These progenitor models feature the 2D modelling of oxygen-flame propagation until the onset of core collapse. We perform axisymmetric simulations with six progenitor models that, at the time of collapse, span a range of propagating flame front radii. For comparison, we also perform a simulation with the same set-up using the canonical, spherically symmetrical progenitor model n8.8. We found that the variations in the progenitor models inherited from simulations of stellar evolution and flame propagation do not significantly alter the global properties of the neutrino-driven ECSN explosion, such as the explosion energy (∼1.36–1.48 × 10⁵⁰ erg) and the mass (∼0.017–0.018 M_⊙) and composition of the ejecta. Due to aspherical perturbations induced by the 2D flame, the ejecta contains a small amount (≲ 1.8 × 10⁻³ M_⊙) of low-Ye (0.35 < Yₑ < 0.4) component. The baryonic mass of the protoneutron star is ∼1.34 M_⊙ (∼1.357 M_⊙) with the new (n8.8) progenitor models when simulations end at ∼400 ms and the discrepancy is due to updated weak-interaction rates in the progenitor evolutionary simulations. Our results reflect the nature of ECSN progenitors containing a strongly degenerate oxygen–neon–magnesium (ONeMg) core and suggest a standardized ECSN explosion initialized by ONeMg core collapse. Moreover, we carry out a rudimentary three-dimensional simulation and find that the explosion properties are fairly compatible with the 2D counterpart. Our paper facilitates a more thorough understanding of ECSN explosions following the ONeMg core collapse, though more three-dimensional simulations are still needed.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stac1035DOIArticle
https://arxiv.org/abs/2112.15257arXivDiscussion Paper
https://doi.org/10.5281/zenodo.5748457DOICSN progenitor models
ORCID:
AuthorORCID
Zha, Shuai0000-0001-6773-7830
O’Connor, Evan P.0000-0002-8228-796X
Couch, Sean M.0000-0002-5080-5996
Leung, Shing-Chi0000-0002-4972-3803
Nomoto, Ken’ichi0000-0001-9553-0685
Additional Information:© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) Accepted 2022 April 9. Received 2022 March 20; in original form 2021 December 23. This work was supported by the Swedish Research Council (Project No. 2020-00452). The simulations were enabled by resources provided by the Swedish National Infrastructure for Computing (SNIC) at PDC and NSC partially funded by the Swedish Research Council through grant agreement no. 2016-07213. SCL acknowledges support by NASA grants HST-946AR-15021.001-A and 80NSSC18K1017. KN was supported by the World Premier International Research Center Initiative (WPI), MEXT, Japan, and the Japan Society for the Promotion of Science (JSPS) KAKENHI grant JP17K05382, JP20K04024, andJP21H04499. SMC was supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics, Early Career Research Program under award number DE-SC0015904. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of Advanced Scientific Computing Research and Office of Nuclear Physics, Scientific Discovery through Advanced Computing (SciDAC) programme under award number DE- SC0017955. This work was supported by the Exascale Computing Project (17-SC-20-SC), a collaborative effort of the U.S. Department of Energy Office of Science and the National Nuclear Security Administration. DATA AVAILABILITY. The ECSN progenitor models used in this work are publicly available at https://doi.org/10.5281/zenodo.5748457. Results of the hydrodynamic simulations will be shared on reasonable request to the corresponding author.
Group:TAPIR
Funders:
Funding AgencyGrant Number
Swedish Research Council2020-00452
Swedish Research Council2016-07213
NASAHST-946AR-15021.001-A
NASA80NSSC18K1017
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP17K05382
Japan Society for the Promotion of Science (JSPS)JP20K04024
Japan Society for the Promotion of Science (JSPS)JP21H04499
Department of Energy (DOE)DE-SC0015904
Department of Energy (DOE)DE-SC0017955
Department of Energy (DOE)17-SC-20-SC
Subject Keywords:hydrodynamics, stars: neutron, supernovae: general
Issue or Number:1
DOI:10.1093/mnras/stac1035
Record Number:CaltechAUTHORS:20220525-90854000
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220525-90854000
Official Citation:Shuai Zha, Evan P O’Connor, Sean M Couch, Shing-Chi Leung, Ken’ichi Nomoto, Hydrodynamic simulations of electron-capture supernovae: progenitor and dimension dependence, Monthly Notices of the Royal Astronomical Society, Volume 513, Issue 1, June 2022, Pages 1317–1328, https://doi.org/10.1093/mnras/stac1035
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:114918
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:31 May 2022 15:56
Last Modified:31 May 2022 15:56

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