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Title: SN Ia Explosions from Hybrid Carbon–Oxygen–Neon White Dwarf Progenitors that Have Mixed during Cooling

Abstract

© 2019. The American Astronomical Society. All rights reserved. The creation of "hybrid" white dwarfs, made of a C-O core within an O-Ne shell has been proposed, and studies indicate that ignition in the C-rich central region makes these viable progenitors for thermonuclear (type Ia) supernovae. Recent work found that the C-O core is mixed with the surrounding O-Ne as the white dwarf cools prior to accretion, which results in lower central C fractions in the massive progenitor than previously assumed. To further investigate the efficacy of hybrid white dwarfs as progenitors of thermonuclear supernovae, we performed simulations of thermonuclear supernovae from a new series of hybrid progenitors that include the effects of mixing during cooling. The progenitor white dwarf model was constructed with the one-dimensional stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA) and represented a star evolved through the phase of unstable interior mixing followed by accretion until it reached conditions for the ignition of carbon burning. This MESA model was then mapped to a two-dimensional initial condition for explosions simulated with FLASH. For comparison, similar simulations were performed for a traditional C-O progenitor white dwarf. By comparing the yields of the explosions, we find that,more » as with earlier studies, the lower C abundance in the hybrid progenitor compared to the traditional C-O progenitor leads to a lower average yield of 56Ni. Although the unmixed hybrid white dwarf showed a similar decrement also in total iron-group yield, the mixed case does not and produces a smaller fraction of iron-group elements in the form of 56Ni. We attribute this to the higher central density required for ignition and the location, center or off-center, of deflagration ignition.« less

Authors:
ORCiD logo [1]; ORCiD logo [2];  [3]; ORCiD logo [1]; ORCiD logo [4]
+ Show Author Affiliations
  1. Univ. of Alabama, Tuscaloosa, AL (United States)
  2. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  3. Univ. of California, Santa Barbara, CA (United States)
  4. Stony Brook Univ., NY (United States)
Publication Date:
Research Org.:
Stony Brook Univ., NY (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF)
OSTI Identifier:
1593806
Alternate Identifier(s):
OSTI ID: 1603565
Report Number(s):
arXiv:1910.12403v1
Journal ID: ISSN 1538-4357; TRN: US2101712
Grant/Contract Number:  
FG02-87ER40317; AST-1211563; AC02-05CH11231
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 887; Journal Issue: 2; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Explosive nucleosynthesis; Type Ia supernovae; Hydrodynamical simulations; White dwarf stars

Citation Formats

Augustine, Carlyn N., Willcox, Donald E., Brooks, Jared, Townsley, Dean M., and Calder, Alan C. SN Ia Explosions from Hybrid Carbon–Oxygen–Neon White Dwarf Progenitors that Have Mixed during Cooling. United States: N. p., 2019. Web. doi:10.3847/1538-4357/ab511a.
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Augustine, Carlyn N., Willcox, Donald E., Brooks, Jared, Townsley, Dean M., & Calder, Alan C. SN Ia Explosions from Hybrid Carbon–Oxygen–Neon White Dwarf Progenitors that Have Mixed during Cooling. United States. https://doi.org/10.3847/1538-4357/ab511a
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Augustine, Carlyn N., Willcox, Donald E., Brooks, Jared, Townsley, Dean M., and Calder, Alan C. Wed . "SN Ia Explosions from Hybrid Carbon–Oxygen–Neon White Dwarf Progenitors that Have Mixed during Cooling". United States. https://doi.org/10.3847/1538-4357/ab511a. https://www.osti.gov/servlets/purl/1593806.
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@article{osti_1593806,
title = {SN Ia Explosions from Hybrid Carbon–Oxygen–Neon White Dwarf Progenitors that Have Mixed during Cooling},
author = {Augustine, Carlyn N. and Willcox, Donald E. and Brooks, Jared and Townsley, Dean M. and Calder, Alan C.},
abstractNote = {© 2019. The American Astronomical Society. All rights reserved. The creation of "hybrid" white dwarfs, made of a C-O core within an O-Ne shell has been proposed, and studies indicate that ignition in the C-rich central region makes these viable progenitors for thermonuclear (type Ia) supernovae. Recent work found that the C-O core is mixed with the surrounding O-Ne as the white dwarf cools prior to accretion, which results in lower central C fractions in the massive progenitor than previously assumed. To further investigate the efficacy of hybrid white dwarfs as progenitors of thermonuclear supernovae, we performed simulations of thermonuclear supernovae from a new series of hybrid progenitors that include the effects of mixing during cooling. The progenitor white dwarf model was constructed with the one-dimensional stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA) and represented a star evolved through the phase of unstable interior mixing followed by accretion until it reached conditions for the ignition of carbon burning. This MESA model was then mapped to a two-dimensional initial condition for explosions simulated with FLASH. For comparison, similar simulations were performed for a traditional C-O progenitor white dwarf. By comparing the yields of the explosions, we find that, as with earlier studies, the lower C abundance in the hybrid progenitor compared to the traditional C-O progenitor leads to a lower average yield of 56Ni. Although the unmixed hybrid white dwarf showed a similar decrement also in total iron-group yield, the mixed case does not and produces a smaller fraction of iron-group elements in the form of 56Ni. We attribute this to the higher central density required for ignition and the location, center or off-center, of deflagration ignition.},
doi = {10.3847/1538-4357/ab511a},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 887,
place = {United States},
year = {2019},
month = {12}
}
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Neutronization During Type Ia Supernova Simmering
text, January 2007

The Reduction of the Electron Abundance during the Pre-explosion Simmering in White Dwarf Supernovae
text, January 2008

High-resolution Smoothed Particle Hydrodynamics simulations of the merger of binary white dwarfs
text, January 2009

On Type Ia Supernovae From The Collisions of Two White Dwarfs
text, January 2009

On variations of the brightness of type Ia supernovae with the age of the host stellar population
text, January 2010

Towards an understanding of Type Ia supernovae from a synthesis of theory and observations
preprint, January 2013

The birth rate of SNe Ia from hybrid CONe white dwarfs
text, January 2014

The hybrid CONe WD + He star scenario for the progenitors of type Ia supernovae
text, January 2014

Single-Degenerate Type Ia Supernovae Are Preferentially Overluminous
text, January 2015

AM Canum Venaticorum Progenitors with Helium Star Donors and the resultant Explosions
preprint, January 2015

Carbon Shell or Core Ignitions in White Dwarfs Accreting from Helium Stars
text, January 2016

Explosion of white dwarfs harboring hybrid CONe cores
text, January 2016

Turbulent Chemical Diffusion in Convectively Bounded Carbon Flames
text, January 2016

Cosmic Chandlery with Thermonuclear Supernovae
text, January 2016

Sub-Chandrasekhar-mass white dwarf detonations revisited
text, January 2017

Double Detonations with Thin, Modestly Enriched Helium Layers Can Make Normal Type Ia Supernovae
text, January 2019

Type Ia Supernova Explosion Models
text, January 2000

Thermonuclear Supernovae: Simulations of the Deflagration Stage and Their Implications
text, January 2002

Signature of Electron Capture in Iron-Rich Ejecta of SN 2003du
text, January 2004

Three-Dimensional Delayed-Detonation Model of Type Ia Supernova
text, January 2004

Capturing the Fire: Flame Energetics and Neutronizaton for Type Ia Supernova Simulations
text, January 2006

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