Cobalt-56 γ-ray emission lines from the type Ia supernova 2014J

@article{Churazov2014Cobalt56E,
  title={Cobalt-56 $\gamma$-ray emission lines from the type Ia supernova 2014J},
  author={E. Churazov and R. Sunyaev and J. Isern and J. Kn{\"o}dlseder and P. Jean and F. Lebrun and N. Chugai and S. Grebenev and E. Bravo and S. Sazonov and M. Renaud},
  journal={Nature},
  year={2014},
  volume={512},
  pages={406-408}
}
A type Ia supernova is thought to be a thermonuclear explosion of either a single carbon–oxygen white dwarf or a pair of merging white dwarfs. The explosion fuses a large amount of radioactive 56Ni (refs 1–3). After the explosion, the decay chain from 56Ni to 56Co to 56Fe generates γ-ray photons, which are reprocessed in the expanding ejecta and give rise to powerful optical emission. Here we report the detection of 56Co lines at energies of 847 and 1,238 kiloelectronvolts and a γ-ray continuum… Expand
FIRST DETECTION OF 56 CO GAMMA-RAY LINES FROM TYPE IA SUPERNOVA (SN2014J) WITH INTEGRAL.
We report the rst ever detection of 56 Co lines at 847 and 1237 keV and a continuum in the 200-400 keV band from the Type Ia supernova SN2014J in M82 with INTEGRAL observatory. The data were takenExpand
Gamma rays from a supernova of type Ia: SN2014J
SN2014J is the closest supernova of type Ia that occurred in the last 40 years. This provides an opportunity for unprecedented observational detail and coverage in many astronomical bands, which willExpand
Gamma-ray line diagnostics of supernova explosions - SN2014J and Cas A
Gamma-rays from nuclear de-excitation of newly procuced isotopes during supernovae (SNe) provide a unique window to the explosion mechanisms. SNe interiors are accessible only by γ-rays as they areExpand
Gamma-ray line measurements from supernova explosions
  • R. Diehl
  • Physics
  • Proceedings of the International Astronomical Union
  • 2017
Abstract Gamma ray lines are expected to be emitted as part of the afterglow of supernova explosions, because radioactive decay of freshly synthesised nuclei occurs. Significant radioactive gamma rayExpand
Astrophysics: Supernova seen through γ-ray eyes
TLDR
The first ever detection of cobalt-56 γ-ray emission lines from a type Ia supernova, SN 2014J, is reported, in broad agreement with the classic model of a white dwarf explosion massive enough to be unstable to gravitational collapse, but do not exclude more complicated merger scenarios. Expand
A likely inverse-Compton emission from the Type IIb SN 2013df
TLDR
The discovery of a hard X-ray source that is associated with a Type II-b supernova and new evidence of the inverse-Compton emission during the early phase of a supernova is reported. Expand
Measuring nickel masses in Type Ia supernovae using cobalt emission in nebular phase spectra
The light curves of Type Ia supernovae (SNe Ia) are powered by the radioactive decay of 56Ni to 56Co at early times, and the decay of 56Co to 56Fe from ?60 d after explosion. We examine the evolutionExpand
5.9-keV Mn K-shell X-ray luminosity from the decay of 55Fe in Type Ia supernova models
We show that the X-ray line flux of the Mn Ka line at 5.9 keV from the decay of Fe-55 is a promising diagnostic to distinguish between Type Ia supernova (SN Ia) explosion models. Using radiationExpand
Radioactive decay products in neutron star merger ejecta: heating efficiency and γ-ray emission
The radioactive decay of the freshly synthesized r-process nuclei ejected in compact binary mergers powers optical/infrared macronovae (kilonovae) that follow these events. The light curves dependExpand
The puzzling early detection of low velocity 56Ni decay lines in SN 2014J: Hints of a compact remnant
We show that the low-velocity 56Ni decay lines detected earlier than expected in the type Ia SN 2014J find an explanation in the Quark-Nova Ia model which involves the thermonuclear explosion of aExpand
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References

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Expectations for the Hard X-ray Continuum and Gamma-ray Line Fluxes from the Type Ia supernova SN 2014J in M82
The hard X-ray continuum and gamma-ray lines from a Type Ia supernova dominate its integrated photon emissions and can provide unique diagnostics of the mass of the ejecta, the 56Ni yield and spatialExpand
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TLDR
It is concluded that no more than about five per cent of type Ia supernovae in early-type galaxies can be produced by white dwarfs in accreting binary systems, unless their progenitors are much younger than the bulk of the stellar population in these galaxies, or explosions of sub-Chandrasekharwhite dwarfs make a significant contribution to the supernova rate. Expand
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We analysed archival data of Chandra pre-explosion observations of the position of SN2014J in M82. No X-ray source at this position was detected in the data, and we calculated upper limits on theExpand
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Type Ia Supernovae from Merging White Dwarfs. I. Prompt Detonations
Merging white dwarfs are a possible progenitor of Type Ia supernovae (SNe Ia). While it is not entirely clear if and when an explosion is triggered in such systems, numerical models suggest that aExpand
Explosion Models for Type IA Supernovae: A Comparison with Observed Light Curves, Distances, H 0, and Q 0
Theoretical monochromatic light curves and photospheric expansion velocities are compared with observations of 27 Type Ia supernovae (SNe Ia). A set of 37 models has been considered which encompassesExpand
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