| dc.creator |
Kashyap, R |
|
| dc.creator |
Haque, T |
|
| dc.creator |
Lorén-Aguilar, P |
|
| dc.creator |
García-Berro, E |
|
| dc.creator |
Fisher, RT |
|
| dc.date |
2018-11-19T14:18:12Z |
|
| dc.date |
2018-12-19 |
|
| dc.date.accessioned |
2022-05-27T01:02:05Z |
|
| dc.date.available |
2022-05-27T01:02:05Z |
|
| dc.identifier |
Vol. 869 (2). Published online 19 December 2018. |
|
| dc.identifier |
10.3847/1538-4357/aaedb7 |
|
| dc.identifier |
http://hdl.handle.net/10871/34821 |
|
| dc.identifier |
1538-4357 |
|
| dc.identifier |
Astrophysical Journal |
|
| dc.identifier.uri |
http://localhost:8080/xmlui/handle/CUHPOERS/241872 |
|
| dc.description |
This is the author accepted manuscript. The final version is available from the American Astronomical Society via the DOI in this record. |
|
| dc.description |
Type Ia supernovae (SNe Ia) originate from the thermonuclear explosion of carbon-oxygen white
dwarfs (CO WDs), giving rise to luminous optical transients. A relatively common variety of subluminous
SNe Ia events, referred to as SNe Iax, are believed to arise from the failed detonation of a
CO WD. In this paper, we explore failed detonation SNe Ia in the context of the double-degenerate
channel of merging white dwarfs. In particular, we have carried out the first fully three-dimensional
simulation of the merger of a ONe WD with a CO WD. While the hot, tidally-disrupted carbon-rich
disk material originating from the CO WD secondary is readily susceptible to detonation in such a
merger, the ONe WD primary core is not. This merger yields a failed detonation, resulting in the ejection
of a small amount of mass, and leaving behind a kicked, super-Chandrasekhar ONe WD remnant
enriched by the fallback of the products of nuclear burning. The resulting outburst is a rapidly-fading
optical transient with a small amount of radioactive 56Ni powering the light curve. Consequently, the
ONe-CO WD merger naturally produces a very faint and rapidly-fading transient, fainter even than
the faintest Type Iax events observed to date, such as SN 2008ha and SN 2010ae. More massive ONe
primaries than considered here may produce brighter and longer-duration transients. |
|
| dc.description |
The work
of P.L-A. and E.G.-B. was partially funded by the
MINECO AYA2014-59084-P grant and by the AGAUR.
RTF thanks the Institute for Theory and Computation
at the Harvard-Smithsonian Center for Astrophysics for
visiting support during which a portion of this work was
undertaken. RTF acknowledges support from NASA
80NSSC18K1013. This work used the Extreme Science
and Engineering Discovery Environment (XSEDE)
Stampede 2 supercomputer at the University of Texas at
Austin’s Texas Advanced Computing Center through allocation
TG-AST100038, supported by National Science
Foundation grant number ACI-1548562 (Towns et al.
2014). |
|
| dc.language |
en |
|
| dc.publisher |
American Astronomical Society |
|
| dc.rights |
© 2018, The American Astronomical Society. All rights reserved. |
|
| dc.title |
Double-Degenerate Carbon-Oxygen and Oxygen-Neon White Dwarf Mergers: A New Mechanism for Faint and Rapid Type Ia Supernovae |
|
| dc.type |
Article |
|