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Reconciling ^(56)Ni Production in Type Ia Supernovae with Double Degenerate Scenarios

Piro, Anthony L. and Thompson, Todd A. and Kochanek, Christopher S. (2014) Reconciling ^(56)Ni Production in Type Ia Supernovae with Double Degenerate Scenarios. Monthly Notices of the Royal Astronomical Society, 438 (4). pp. 3456-3464. ISSN 0035-8711.

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We combine the observed distribution of Type Ia supernova (SN Ia) ^(56)Ni yields with the results of sub-Chandrasekhar detonation and direct collision calculations to estimate what mass white dwarfs (WDs) should be exploding for each scenario. For collisions, the average exploding WD mass must be peaked at ≈0.75M_☉, significantly higher than the average field WD mass of ≈0.55–0.60M_☉. Thus, if collisions produce most SNe Ia, then a mechanism must exist that favours higher mass WDs. On the other hand, in old stellar populations, collisions would naturally result in low-luminosity SNe Ia, and we suggest these may be related to 1991bg-like events. For sub-Chandrasekhar detonations, the average exploding WD mass must be peaked at ≈1.1M_☉. This is similar to the average total mass in WD–WD binaries, but it is not clear whether double degenerate mergers would synthesize sufficient ^(56)Ni to match observed yields. If not, then actual ≈1.1M_☉ WDs would be needed for sub-Chandrasekhar detonations. Since such high-mass WDs are produced relatively quickly in comparison to the age of SN Ia environments, this would require either accretion on to lower mass WDs prior to ignition or a long time-scale between formation of the ≈1.1M_☉ WD and ignition.

Item Type:Article
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URLURL TypeDescription Paper
Piro, Anthony L.0000-0001-6806-0673
Kochanek, Christopher S.0000-0001-6017-2961
Additional Information:© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 December 18. Received 2013 December 18; in original form 2013 September 11. Advance Access publication 2014 January 14. We thank Subo Dong for comments on a previous draft, which helped us improve our ^(56)Ni yield estimates. We also thank Ashley Ruiter for discussions about population synthesis models and sharing her work for comparison. We thank Carles Badenes, Ryan Foley, Mohan Ganeshalingam, Peter Garnavich, Saurabh Jha, Christian Ott, Ben Shappee and Ken Shen for helpful feedback and assistance with interpreting observations. We also thank the Center for Cosmology and Astro-Particle Physics for funding ALP’s visit to Ohio State University, where this work germinated. ALP thanks John Beacom for generously arranging his visit. ALP is supported through NSF grants AST-1205732, PHY-1068881, PHY-1151197 and the Sherman Fairchild Foundation. TAT is supported in part by NSF grant AST-1313252.
Funding AgencyGrant Number
Center for Cosmology and AstroParticle Physics (CCAPP)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Subject Keywords:nuclear reactions, nucleosynthesis, abundances; supernovae: general; white dwarfs
Issue or Number:4
Record Number:CaltechAUTHORS:20130819-084840899
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Official Citation:Piro, A. L., Thompson, T. A., & Kochanek, C. S. (2014). Reconciling 56Ni production in Type Ia supernovae with double degenerate scenarios. Monthly Notices of the Royal Astronomical Society, 438(4), 3456-3464. doi: 10.1093/mnras/stt2451
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:40718
Deposited By: Tony Diaz
Deposited On:19 Aug 2013 21:50
Last Modified:05 Nov 2019 00:48

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