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 »
- Authors:
-
[1];
[2];
[1];
[4]
- Univ. of Alabama, Tuscaloosa, AL (United States)
- Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
- Univ. of California, Santa Barbara, CA (United States)
- 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
- 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.
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. doi:10.3847/1538-4357/ab511a.
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. doi:10.3847/1538-4357/ab511a. https://www.osti.gov/servlets/purl/1593806.
@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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