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Chemical Yields from Supernovae and Hypernovae

Published online by Cambridge University Press:  01 June 2008

Ken'ichi Nomoto ,
Shinya Wanajo ,
Yasuomi Kamiya ,
Nozomu Tominaga  and
Hideyuki Umeda
Ken'ichi Nomoto
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-85668, Japan email: nomoto@astron.s.u-tokyo.ac.jp Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
Shinya Wanajo
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-85668, Japan email: nomoto@astron.s.u-tokyo.ac.jp Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
Yasuomi Kamiya
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-85668, Japan email: nomoto@astron.s.u-tokyo.ac.jp Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
Nozomu Tominaga
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 113-0033, Japan
Hideyuki Umeda
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
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Abstract

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We review the final stages of stellar evolution, supernova properties, and chemical yields as a function of the progenitor's mass. (1) 8 - 10 M⊙ stars are super-AGB stars when the O+Ne+Mg core collapses due to electron capture. These AGB-supernovae may constitute an SN 2008S-like sub-class of Type IIn supernovae. These stars produce little α-elements and Fe-peak elements, but are important sources of Zn and light p-nuclei. (2) 10 - 90 M⊙ stars undergo Fe-core collapse. Nucleosynthesis in aspherical explosions is important, as it can well reproduce the abundance patterns observed in extremely metal-poor stars. (3) 90 - 140 M⊙ stars undergo pulsational nuclear instabilities at various nuclear burning stages, including O and Si-burning. (4) Very massive stars with M ≳ 140 M⊙ either become pair-instability SNe, or undergo core-collapse to form intermediate mass black holes if the mass loss is small enough.

Keywords

Galaxy: halo — gamma rays: bursts — nuclear reactionsnucleosynthesisabundances — stars: abundances — stars: AGB — supernovae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S254: The Galaxy Disk in Cosmological Context , June 2008 , pp. 355 - 368
Copyright
Copyright © International Astronomical Union 2009

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