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Nucleosynthesis in Type I Supernovae: Carbon Deflagration and Helium Detonation Models

  • Ken’ichi Nomoto
Part of the Astrophysics and Space Science Library book series (ASSL, volume 109)

Abstract

The evolution of accreting white dwarfs in close binary systems is studied from the onset of accretion through the thermonuclear explosion. Relatively rapid accretion onto C+O white dwarfs leads to a carbon deflagration supernova which disrupts the star completely. Explosive nucleosynthesis in the deflagration wave produces 0.5–0.6 M⊙ 56 Ni in the inner part of the star; this amount of 56Ni is sufficient to power the light curve of Type I supernovae by the radioactive decays. In the outer layers of the star, the deflagration wave synthesizes appreciable amount of intermediate mass elements such as Ca, Ar, S, Si, Mg, and O; this is consistent with the spectra of Type I supernovae near maximum light. Thus the carbon deflagration model can account for many of the observed features. Moreover, the nuclear products in this model are quite complementary to nucleosynthesis in Type II supernovae.

On the other hand, slow accretion results in the detonation supernova explosion, namely, a helium detonation in helium white dwarfs and double or single detonations in C+O white dwarfs. This type of explosion produces almost exclusively iron peak elements and thus cannot account for the observed features of Type I supernovae.

Possible progenitors of Type I supernovae are discussed, namely, white dwarfs undergoing hydrogen burning near the surface and double white dwarf systems undergoing transfer of helium or C+O onto the more massive white dwarf.

Keywords

Detonation Wave Accretion Rate White Dwarf Asymptotic Giant Branch Deflagration Wave 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© D. Reidel Publishing Company 1984

Authors and Affiliations

  • Ken’ichi Nomoto
    • 1
    • 2
  1. 1.Dept. of Earth Science and Astronomy, College of Arts and SciencesUniversity of TokyoMeguro-ku, Tokyo 153Japan
  2. 2.Max-Planck-Institut für Physik und AstrophysikInstitut für AstrophysikGarching b. MünchenGermany

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