The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star

@article{Howell2006TheTI,
  title={The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star},
  author={D. Andrew Howell and Mark Sullivan and Peter E. Nugent and Richard S. Ellis and Alex Conley and Damien le Borgne and Raymond G. Carlberg and Julien Guy and David D. Balam and S. Basa and Dominique Fouchez and Isobel M. Hook and Eric Y. Hsiao and James D. Neill and R. Pain and Kathryn Perrett and C. Pritchet},
  journal={Nature},
  year={2006},
  volume={443},
  pages={308-311}
}
The accelerating expansion of the Universe, and the need for dark energy, were inferred from observations of type Ia supernovae. There is a consensus that type Ia supernovae are thermonuclear explosions that destroy carbon–oxygen white dwarf stars that have accreted matter from a companion star, although the nature of this companion remains uncertain. These supernovae are thought to be reliable distance indicators because they have a standard amount of fuel and a uniform trigger: they are… 

Astronomy: Champagne supernova

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References

SHOWING 1-10 OF 38 REFERENCES

Could There Be a Hole in Type Ia Supernovae?

In the favored progenitor scenario, Type Ia supernovae (SNe Ia) arise from a white dwarf accreting material from a nondegenerate companion star. Soon after the white dwarf explodes, the ejected

Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant

We present spectral and photometric observations of 10 Type Ia supernovae (SNe Ia) in the redshift range 0.16 ≤ z ≤ 0.62. The luminosity distances of these objects are determined by methods that

The Hubble Constant from Nickel Radioactivity in Type IA Supernovae

On the assumptions that Type Ia supernovae are thermonuclear disruptions of carbon-oxygen white dwarfs near the Chandrasekhar mass, that their light curves are powered by the radioactive decay of 56

Accreting white dwarf models for type I supernovae. III. Carbon deflagration supernovae

The carbon deflagration models in accreting C+O white dwarfs are presented as a plausible model for Type I supernovae. The evolution of the white dwarf is calculated from the beginning of accretion.

ON THE SPECTRUM AND NATURE OF THE PECULIAR TYPE IA SUPERNOVA 1991T

A parametrized supernova synthetic-spectrum code is used to study line identifications in the photospheric-phase spectra of the peculiar Type Ia SN 1991T, and to extract some constraints on the

Rates and Properties of Type Ia Supernovae as a Function of Mass and Star Formation in Their Host Galaxies

We show that Type Ia supernovae (SNe Ia) are formed within both very young and old stellar populations, with observed rates that depend on the stellar mass and mean star formation rates (SFRs) of

The Rise Time of Type Ia Supernovae from the Supernova Legacy Survey

We compare the rise times of nearby and distant Type Ia supernovae (SNe Ia) as a test for evolution using 73 high-redshift spectroscopically confirmed SNe Ia from the first 2 years of the 5 year

On the evolution of rapidly rotating massive white dwarfs towards supernovae or collapses

A recent study indicated that the inner cores of rapidly accreting (M > 10 -7 M ○. yr -1 ) CO white dwarfs may rotate differentially, with a shear fate near the threshold value for the onset of the

Type I supernovae. I. Analytic solutions for the early part of the light curve

Analytic solutions for light curves, effective temperatures, and broad-band colors of Type I supernovae are presented. The method is generalized to include effects of finite (large) initial radius

The Physics of Supernova Explosions

The modern study of supernovae involves many aspects: presupernova stellar evolution, the physics of the explosions themselves, observations at all wavelengths of the outbursts and their remnants,