Super- and massive AGB stars - IV. Final fates initial-to-final mass relation
We explore the final fates of massive intermediate-mass stars by computing detailed stellar models from the zero-age main sequence until near the end of the thermally pulsing phase. These super-asymptotic giant branch (super-AGB) and massive AGB star models are in the mass range between 5.0 and 10.0...
| Autores: | , , , , |
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| Formato: | artículo |
| Fecha de publicación: | 2015 |
| País: | España |
| Recursos: | Universitat Politècnica de Catalunya (UPC) |
| Repositorio: | UPCommons. Portal del coneixement obert de la UPC |
| Idioma: | inglés |
| OAI Identifier: | oai:upcommons.upc.edu:2117/27811 |
| Acesso em linha: | https://hdl.handle.net/2117/27811 https://dx.doi.org/10.1093/mnras/stu2180 |
| Access Level: | acceso abierto |
| Palavra-chave: | White dwarf stars Supernovae stars AGB and post-AGB stars evolution-supernovae general-white dwarfs ASYMPTOTIC GIANT BRANCH ELECTRON-CAPTURE SUPERNOVAE EXTREMELY METAL-POOR CORE-COLLAPSE SUPERNOVAE CIRCLE DOT MODEL S-PROCESS NUCLEOSYNTHESIS CLOSE BINARY-SYSTEMS DREDGE-UP PHASE NE-MG CORES INTERMEDIATE-MASS Estels nans Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| Resumo: | We explore the final fates of massive intermediate-mass stars by computing detailed stellar models from the zero-age main sequence until near the end of the thermally pulsing phase. These super-asymptotic giant branch (super-AGB) and massive AGB star models are in the mass range between 5.0 and 10.0 M circle dot for metallicities spanning the range Z = 0.02-0.0001. We probe the mass limits M-up, M-n and M-mass, the minimum masses for the onset of carbon burning, the formation of a neutron star and the iron core-collapse supernovae, respectively, to constrain the white dwarf/electron-capture supernova (EC-SN) boundary. We provide a theoretical initial-to-final mass relation for the massive and ultra-massive white dwarfs and specify the mass range for the occurrence of hybrid CO(Ne) white dwarfs. We predict EC-SN rates for lower metallicities which are significantly lower than existing values from parametric studies in the literature. We conclude that the EC-SN channel (for single stars and with the critical assumption being the choice of mass-loss rate) is very narrow in initial mass, at most approximate to 0.2 M circle dot. This implies that between 2 and 5 per cent of all gravitational collapse supernova are EC-SNe in the metallicity range Z = 0.02-0.0001. With our choice for mass-loss prescription and computed core growth rates, we find, within our metallicity range, that CO cores cannot grow sufficiently massive to undergo a Type 1.5 SN explosion. |
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