Journal
SCIENCE
Volume 345, Issue 6201, Pages 1162-1165Publisher
AMER ASSOC ADVANCEMENT SCIENCE
DOI: 10.1126/science.1254738
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Funding
- Deutsche Forschungsgemeinschaft (DFG) cluster of excellence Origin and Structure of the Universe and from DFG Transregio [33]
- Russian Academy of Sciences [RAS P-21]
- DFG [RO3676/1-1]
- ARCHES prize of the German Ministry for Education and Research
- Japan Society for the Promotion of Science [23740141, 26800100]
- WPI, at the Ministry of Education, Culture, Sports. Science Technology
- Grants-in-Aid for Scientific Research [26800100] Funding Source: KAKEN
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Type Ia supernovae result from binary systems that include a carbon-oxygen white dwarf, and these thermonuclear explosions typically produce 0.5 solar mass of radioactive Ni-56. The Ni-56 is commonly believed to be buried deeply in the expanding supernova cloud. In SN2014J, we detected the lines at 158 and 812 kiloelectron volts from Ni-56 decay (time similar to 8.8 days) earlier than the expected several-week time scale, only similar to 20 days after the explosion and with flux levels corresponding to roughly 10% of the total expected amount of Ni-56. Some mechanism must break the spherical symmetry of the supernova and at the same time create a major amount of Ni-56 at the outskirts. A plausible explanation is that a belt of helium from the companion star is accreted by the white dwarf, where this material explodes and then triggers the supernova event.
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