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Nucleosynthesis of the Elements in Faint Supernovae and Hypernovae

Published online by Cambridge University Press:  09 March 2010

Ken'ichi Nomoto ,
Takashi Moriya  and
Nozomu Tominaga
Ken'ichi Nomoto
Affiliation:
Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, Kashiwanoha 5-1-5, Kashiwa, Chiba 277-8583, Japan email: nomoto@astron.s.u-tokyo.ac.jp Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
Takashi Moriya
Affiliation:
Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, Kashiwanoha 5-1-5, Kashiwa, Chiba 277-8583, Japan email: nomoto@astron.s.u-tokyo.ac.jp Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
Nozomu Tominaga
Affiliation:
Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, Kashiwanoha 5-1-5, Kashiwa, Chiba 277-8583, Japan email: nomoto@astron.s.u-tokyo.ac.jp Department of Physics, Konan University, Okamoto, Kobe 658-8501, Japan
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Abstract

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We review the properties of supernovae (SNe) as a function of the progenitor's mass M. (1) Mup - 10 M⊙ stars are super-AGB stars and resultant electron capture SNe may be Faint supernovae like Type IIn SN 2008S. (2) 10 - 12 M⊙ stars undergo Fe-core collapse to form neutron stars (NSs) and Faint supernovae. (3) 12 M⊙ - MBN stars undergo Fe-core collapse to form NSs and normal core-collapse supernovae. (4) MBN - 90 M⊙ stars undergo Fe-core collapse to form Black Holes. Resultant supernovae are bifurcate into Hypernovae and Faint supernovae. The observed properties of SN 2008ha can be explained with this type of Faint supernovae. (5) 90 - 140 M⊙ stars produce Luminous SNe, like SNe 2007bi and 2006gy. (6) 140 - 300 M⊙ stars become pair-instability supernovae which could be Luminous supernovae (SNe 2007bi and 2006gy). (7) Very massive stars with M ≳ 300 M⊙ undergo core-collapse to form intermediate mass black holes. Some SNe could be more Luminous supernovae (like SN 2006gy).

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 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 34 - 41
Copyright
Copyright © International Astronomical Union 2010

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