Super and massive AGB stars - IV. Final fates - Initial to final mass relation

By C. Doherty, P. Gil-Pons, L. Siess, J. Lattanzio, H. Lau. 2014

188 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/5d896071448740e53bb1be6ca3fee2b73548d696

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Citations in the corpus

Ultra-stripped supernovae: progenitors and fate (2015, background): “The initial masses of our binary stars which produce EC SNe are most likely found in the interval8 − 11 M⊙ (Podsiadlowski et al. 2004; Umeda et al. 2012; Jones et al. 2013, 2014; Takahashi et al. 2013; Doherty et al. 2015, and referenc s therein).”
Formation of Double Neutron Star Systems (2017, background): “As discussed in detail in Podsiadlowski et al. (2004); Poelarends et al. (2008); Takahashi et al. (2013); Jones et al. (2013, 2014); Doherty et al. (2015); Woosley & Heger (2015); Jones et al. (2016); Radice et al. (2017), the ZAMS mass range of isolated stars producing EC SNe is restricted to a…”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “…may also be a route towards core collapse from superAGB stars with O-Ne-Mg cores (Nomoto 1984, 1987; Poelarends et al. 2008; Jones et al. 2013, 2014; Doherty et al. 2015), where rapid core contraction is triggered by electron captures on 20Ne and 24Mg;1 hence this sub-class is designated as…”
New white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 12 (2015, background): “White dwarf stars are the end product of evolution of all stars with progenitor masses below 7–10.6 M⊙, depending on metallicity (e.g Ibeling & Heger 2013; Doherty et al. 2015; Woosley & Heger 2015), which corresponds to over 97% of the total number of stars.”
STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS (2016, background): “Above these masses, stars will become ONe super-AGB stars or neutron stars (Doherty et al. 2015).”
EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF AGB STARS AT DIFFERENT METALLICITIES. III. INTERMEDIATE-MASS MODELS, REVISED LOW-MASS MODELS, AND THE pH-FRUITY INTERFACE (2015, methodology): “– 44 – reported in Doherty et al. (2015)11, the perfect gas equation is adopted for fully ionized regions, the Saha EOS in partially ionized regions (following the method of Bærentzen 1965), while EOS from Beaudet & Tassoul (1971) is used for relativistic or electron-degenerate gas.”
Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction (2017, background): “…to stars with birth masses larger than approximately 8 M (Heger et al. 2003), although the exact value depends on model assumptions concerning core overshooting, stellarwind mass-loss, and metallicity (e.g., Poelarends et al. 2008; Jones et al. 2013; Takahashi et al. 2013; Doherty et al. 2015).”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “Super-AGB stars are interesting in their own right because they occupy the blurry mass boundary within which ONe and ONeMg WDs can form as a consequence of advanced burning in the core (e.g., Doherty et al. 2015).”