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Electron-capture Supernovae of Super-AGB Stars: Sensitivity on Input Physics

Leung, Shing-Chi and Nomoto, Ken’ichi and Suzuki, Tomoharu (2020) Electron-capture Supernovae of Super-AGB Stars: Sensitivity on Input Physics. Astrophysical Journal, 889 (1). Art. No. 34. ISSN 1538-4357. doi:10.3847/1538-4357/ab5d2f.

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Stars of M ~ 8–10 M⊙ on their main sequence form strongly electron-degenerate oxygen–neon–magnesium (ONeMg) cores and become super–asymptotic giant branch stars. If such an ONeMg core grows to 1.38 M⊙, electron captures on ²⁰Ne(e, ν_e) ²⁰F(e, ν_e) ²⁰O take place and ignite O–Ne deflagration around the center. In this work, we perform two-dimensional hydrodynamical simulations of the propagation of the O–Ne flame to see whether such a flame triggers a thermonuclear explosion or induces a collapse of the ONeMg core due to subsequent electron capture behind the flame. We present a series of models to explore how the outcome depends on model parameters for a central density ranging between 10^(9.80) and 10^(10.20) g cm⁻³, flame structures of both centered and off-centered ignition kernels, special and general relativistic effects, turbulent flame speed formulae, and the treatments of laminar burning phase. We obtain bifurcation between the electron-capture induced collapse and thermonuclear explosion depending mainly on the central density. We find that the ONeMg core obtained from stellar evolutionary models has a high tendency to collapse into a neutron star. We discuss the implications of the electron-capture supernovae in chemical evolution and the possible observational signals of this class of supernovae.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Leung, Shing-Chi0000-0002-4972-3803
Nomoto, Ken’ichi0000-0001-9553-0685
Additional Information:© 2020 The American Astronomical Society. Received 2019 January 30; revised 2019 November 26; accepted 2019 November 26; published 2020 January 22. This work was supported by World Premier International Research Center Initiative (WPI), MEXT, Japan, and JSPS KAKENHI grant Nos. JP26400222, JP16H02168, and JP17K05382. S.C.L. also acknowledges funding by the grant HST-AR-15021.001-A. We thank the developers of the stellar evolution code MESA for making the code open-source. We thank the anonymous referee for the very detailed and constructive comments that improved this article. We also thank our colleagues who kindly spent their time to help us improve the writing of this article. We thank F. X. Timmes for his open-source microphysics algorithm including the Helmholtz equation of state subroutine, the torch nuclear reaction network designed for an arbitrary choices of isotopes, the seven-isotope nuclear reaction network. We also thank Ming-Chung Chu for the initial inspiration of building the hydrodynamical code. We also thank H. Shen for her open-source equation of state for the nuclear matter. We thank Christian Ott and Evan O'Connor for the equation of state (EOS) driver for reading the HShen EOS and their open source data for the parameterized electron capture value before bounce. We thank Shuai Zha for his discussion of the preliminary results of his pre-runaway models.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
Japan Society for the Promotion of Science (JSPS)JP26400222
Japan Society for the Promotion of Science (JSPS)JP16H02168
Japan Society for the Promotion of Science (JSPS)JP17K05382
NASA Hubble FellowshipHST-AR-15021.001-A
Subject Keywords:Supernovae; Asymptotic giant branch stars; Hydrodynamical simulations; Neutron stars
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Supernovae (1668); Asymptotic giant branch stars (2100); Hydrodynamical simulations (767); Neutron stars (1108)
Record Number:CaltechAUTHORS:20200122-135946093
Persistent URL:
Official Citation:Shing-Chi Leung et al 2020 ApJ 889 34
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:100848
Deposited By: Tony Diaz
Deposited On:22 Jan 2020 23:12
Last Modified:16 Nov 2021 17:57

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