Physics – Nuclear Physics
Scientific paper
Jun 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1238....9n&link_type=abstract
TOURS SYMPOSIUM ON NUCLEAR PHYSICS AND ASTROPHYSICS-VII. AIP Conference Proceedings, Volume 1238, pp. 9-17 (2010).
Physics
Nuclear Physics
Neutron Stars, Black Holes, Brightness, Stellar Evolution, Neutron Stars, Black Holes, Luminosity And Mass Functions, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages
Scientific paper
We review the properties of supernovae (SNe) as a function of the progenitor's mass M. (1) 8-10 Msolar stars are super-AGB stars and resultant electron capture SNe may be Faint supernovae like Type IIn SN 2008S. (2) 10-13 Msolar stars undergo Fe-core collapse to form neutron stars (NSs) and Faint supernovae. (3) 13 Msolar-MBN stars undergo Fe-core collapse to form NSs and normal core-collapse supernovae. (4) MBN-90 Msolar stars undergo Fe-core collapse to form Black Holes. Resultant supernovae are bifurcate into Hypernovae and Faint supernovae. (5) 90-140 Msolar stars produce Luminous SNe, like SNe 2007 bi and 2006 gy (6) 140-300 Msolar stars become pair-instability supernovae which could be Luminous supernovae (SNe 2007 bi and 2006 gy). (7) Very massive stars with M>~300 Msolar undergo core-collapse to form intermediate mass black holes. Some SNe could be more Luminous supernovae (like SN 2006 gy).
Moriya Takashi
Nomoto Ken'ichi
Tominaga Nozomu
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