TYPE II Supernovae from 8–10 M⊙ Progenitors

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


The evolution of stars in the mass range of 8–12 M⊙ is summarized; it is significantly different from more massive stars (typically a 25 M⊙ star) because of smaller core mass and stronger electron degeneracy. Stars of 10-12 M⊙ undergo strong shell flashes of neon, oxygen, and silicon and the resultant iron core eventually collapse. Stars of 8–10 M⊙ form electron-degenerate O+Ne+Mg cores and undergo collapse induced by electron captures. The collapse of such less massive progenitors does lead to the Type II supernova explosion. Nucleosynthesis in these stars does not contribute much to the galactic nucleosynthesis, but provides useful information on the Crab Nebula’s progenitor.


Massive Star White Dwarf Supernova Explosion Iron Core Carbon Star 
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’icni 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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