Journal
NATURE
Volume 521, Issue 7552, Pages 332-+Publisher
NATURE PUBLISHING GROUP
DOI: 10.1038/nature14455
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Categories
Funding
- Kepler GO3
- GO4 [NNX12AC95G, NNX13AC27G]
- Kepler grants [NNX12AC89G, NNX11AG95G]
- NSF [AST-1211916, GN-2013A-Q-4, GS-2013A-Q-115]
- TABASGO Foundation
- Christopher R. Redlich Fund
- NASA [NAS5-26555]
- NASA Office of Space Science [NNX13AC07G]
- NASA Science Mission directorate
- National Science Foundation (United States)
- National Research Council (Canada)
- CONICYT (Chile)
- Australian Research Council (Australia)
- Ministerio da Ciencia, Tecnologia e Inovacao (Brazil)
- Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina)
- W. M. Keck Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1211916] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1109896] Funding Source: National Science Foundation
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Type Ia supernovae are thought to be the result of a thermonuclear runaway in carbon/oxygen white dwarfs, but it is uncertain whether the explosion is triggered by accretion from a non-degenerate companion star or by a merger with another white dwarf. Observations of a supernova immediately following the explosion provide unique information on the distribution of ejected material(1) and the progenitor system. Models predict(2) that the interaction of supernova ejecta with a companion star or circumstellar debris lead to a sudden brightening lasting from hours to days. Here we present data for three supernovae that are likely to be type Ia observed during the Kepler mission(3) with a time resolution of 30 minutes. We find no signatures of the supernova ejecta interacting with nearby companions. The lack of observable interaction signatures is consistent with the idea that these three supernovae resulted from the merger of binary white dwarfs or other compact stars such as helium stars.
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