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Chemical Yields from Supernovae and Hypernovae
| Content Provider | Semantic Scholar |
|---|---|
| Author | Nomoto, Ken’ichi Wanajo, Shinya Kamiya, Yasuomi Tominaga, Nozomu Umeda, Hideyuki |
| Copyright Year | 2009 |
| Abstract | We review the final stages of stellar evolution, supernova properties, and chemical yields as a function of the progenitor’s mass M . (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 Fepeak 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) 140 300 M⊙ stars become pair-instability supernovae, if the mass loss is small enough. (5) Very massive stars with M ∼ > 300M⊙ undergo core-collapse to form intermediate mass black holes. |
| File Format | PDF HTM / HTML |
| Alternate Webpage(s) | http://arxiv.org/pdf/0901.4536v1.pdf |
| Alternate Webpage(s) | http://arxiv.org/pdf/0901.4536v2.pdf |
| Language | English |
| Access Restriction | Open |
| Subject Keyword | Field electron emission Instability Iron Silicon Stars, Celestial Stellar (payment network) |
| Content Type | Text |
| Resource Type | Article |
