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Super- and massive AGB stars - IV. Final fates initial-to-final mass relation
Doherty, Carolyn L.; Gil Pons, Pilar; Siess, Lionel; Lattanzio, John C.; Lau, Herbert B.
Universitat Politècnica de Catalunya. Departament de Física Aplicada; Universitat Politècnica de Catalunya. CTE-CRAE - Grup de Recerca en Ciències i Tecnologies de l'Espai
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.
Peer Reviewed
Àrees temàtiques de la UPC::Física::Astronomia i astrofísica
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
Attribution-NonCommercial-NoDerivs 3.0 Spain
http://creativecommons.org/licenses/by-nc-nd/3.0/es/
info:eu-repo/semantics/publishedVersion
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