Nucleosynthesis in Chandrasekhar Mass Models for Type Ia Supernovae and Constraints on Progenitor Systems and Burning-Front Propagation

  title={Nucleosynthesis in Chandrasekhar Mass Models for Type Ia Supernovae and Constraints on Progenitor Systems and Burning-Front Propagation},
  author={Koichi Iwamoto and Franziska Brachwitz and Ken’ichi Nomoto and N. Kishimoto and Hideyuki Umeda and W. Raphael Hix and Friedrich-Karl Thielemann},
  journal={The Astrophysical Journal Supplement Series},
  pages={439 - 462}
The major uncertainties involved in the Chandrasekhar mass models for Type Ia supernovae (SNe Ia) are related to the companion star of their accreting white dwarf progenitor (which determines the accretion rate and consequently the carbon ignition density) and the flame speed after the carbon ignition. We calculate explosive nucleosynthesis in relatively slow deflagrations with a variety of deflagration speeds and ignition densities to put new constraints on the above key quantities. The… 

Explosive Nucleosynthesis in Near-Chandrasekhar Mass White Dwarf Models for Type Iax Supernovae: Dependence on Model Parameters

The recently observed diversity of Type Ia supernovae (SNe Ia) has motivated us to conduct the theoretical modeling of SNe Ia for a wide parameter range. In particular, the origin of Type Iax

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Supernovae of both types represent the most important nucleosynthesis contributors to galactic evolution and SNe la represent the major source of Fe-group nuclei. Our theoretical understanding is

Abundance stratification in type Ia supernovae – II. The rapidly declining, spectroscopically normal SN 2004eo

The variation in properties of Type Ia supernovae, the thermonuclear explosions of Chandrasekhar-mass carbon-oxygen white dwarfs, is caused by different nucleosynthetic outcomes of these explosions,

Heavy elements nucleosynthesis on accreting white dwarfs: building seeds for the p-process

The origin of the proton-rich trans-iron isotopes in the solar system is still uncertain. Single-degenerate thermonuclear supernovae (SNIa) with n-capture nucleosynthesis seeds assembled in the

New Type Ia Supernova Yields and the Manganese and Nickel Problems in the Milky Way and Dwarf Spheroidal Galaxies

In our quest to identify the progenitors of Type Ia supernovae (SNe Ia), we first update the nucleosynthesis yields for both near-Chandrasekhar- (Ch) and sub-Ch-mass white dwarfs (WDs) for a wide

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We analyze the nucleosynthesis yields of various Type Ia supernova explosion simulations including pure detonations in sub-Chandrasekhar mass white dwarfs; double detonations and pure helium

Observational Evidence for High Neutronization in Supernova Remnants: Implications for Type Ia Supernova Progenitors

The physical process whereby a carbon–oxygen white dwarf explodes as a Type Ia supernova (SN Ia) remains highly uncertain. The degree of neutronization in SN Ia ejecta holds clues to this process


Despite decades of intense efforts, many fundamental aspects of Type Ia supernovae (SNe Ia) remain elusive. One of the major open questions is whether the mass of an exploding white dwarf (WD) is

Constraining the Single-degenerate Channel of Type Ia Supernovae with Stable Iron-group Elements in SNR 3C 397

Recent Suzaku X-ray spectra of supernova remnant (SNR) 3C 397 indicate enhanced stable iron group element abundances of Ni, Mn, Cr, and Fe. Seeking to address key questions about the progenitor and

Single Degenerate Models for Type Ia Supernovae: Progenitor’s Evolution and Nucleosynthesis Yields

We review how the single degenerate models for Type Ia supernovae (SNe Ia) works. In the binary star system of a white dwarf (WD) and its non-degenerate companion star, the WD accretes either



Nucleosynthesis in type Ia supernovae

Nucleosynthesis in SNE Ia and Their Impact on Galactic Evolution

Spectra and light curves of SNIa events and their appearance in all galaxy types clearly indicate their origin from thermonuclear explosions of white dwarfs. Details of the explosion, i.e.,

Accreting white dwarf models for type I supernovae. I. Presupernova evolution and triggering mechanisms

As a plausible explosion model for a Type I supernova, the evolution of carbon-oxygen white dwarfs accreting helium in binary systems was investigated from the onset of accretion up to the point at

Type Ia Supernovae: Influence of the Initial Composition on the Nucleosynthesis, Light Curves, and Spectra and Consequences for the Determination of ΩM and Λ

The influence of the initial composition of the exploding white dwarf on the nucleosynthesis, light curves, and spectra of Type Ia supernovae has been studied in order to evaluate the size of


We review the candidate progenitor binary systems of Type Ia supernovae (SNe Ia). We argue that the exploding star is likely to be a mass accreting carbon-oxygen white dwarf. "Primary"

Nucleosynthesis in Type II Supernovae and the Abundances in Metal-poor Stars

We explore the effects on nucleosynthesis in Type II supernovae of various parameters (mass cut, neutron excess, explosion energy, progenitor mass) in order to explain the observed trends of the

Carbon ignition in a rapidly accreting degenerate dwarf - A clue to the nature of the merging process in close binaries.

Recent studies have suggested that the merging of two degenerate dwarfs composed of carbon and oxygen and of total mass larger than the Chandrasekhar limit occurs at a frequency comparable to that of

More on carbon burning in electron-degenerate matter: within single stars of intermediate mass and within accreting white dwarfs.

Carbon burning in highly electron-degenerate matter is followed in two astrophysically interesting cases; an intermediate-mass star that, on the asymptotic giant branch, has developed a large

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We propose a new model for progenitor systems of Type Ia supernovae. The model consists of an accreting white dwarf and a lobe-filling, low-mass red giant. When the mass accretion rate exceeds a

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We present our first results from a study of the supernova remnants (SNRs) in the Large Magellanic Cloud (LMC) using data from ASCA. The three remnants we have analyzed to date, 0509-67.5, 0519-69.0,