ADVANCED BURNING STAGES AND FATE OF 8–10 M☉ STARS

@article{Jones2013ADVANCEDBS,
  title={ADVANCED BURNING STAGES AND FATE OF 8–10 M☉ STARS},
  author={S Jones and Raphael Hirschi and Ken’ichi Nomoto and Tobias Fischer and Francis X. Timmes and Falk Herwig and Bill Paxton and Hiroshi Toki and T. L. Suzuki and Gabriel Mart{\'i}nez-Pinedo and Y. H. Lam and M. G. Bertolli},
  journal={The Astrophysical Journal},
  year={2013},
  volume={772}
}
The stellar mass range 8 ≲ M/M☉ ≲ 12 corresponds to the most massive asymptotic giant branch (AGB) stars and the most numerous massive stars. It is host to a variety of supernova (SN) progenitors and is therefore very important for galactic chemical evolution and stellar population studies. In this paper, we study the transition from super-AGB (SAGB) star to massive star and find that a propagating neon–oxygen-burning shell is common to both the most massive electron capture supernova (EC-SN… 
Final evolution of super-AGB stars and supernovae triggered by electron capture
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The post-helium-burning evolution of stars from 7 M ⊙ ?> to 11 M ⊙ ?> is complicated by the lingering effects of degeneracy and off-center ignition. Here, stars in this mass range are studied using a
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Stars in the mass range of 8 to 12 M (solar masses) represent the transition region between those that end their lives producing white dwarfs and those that undergo a core-collapse supernova and
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Context. Most super-asymptotic giant branch (SAGB) stars are expected to end their life as oxygen–neon white dwarfs rather than electron capture supernovae (ECSN). The reason is ascribed to the
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Abstract The chemical evolution of the Universe is governed by the chemical yields from stars, which in turn are determined primarily by the initial stellar mass. Even stars as low as 0.9 M⊙ can, at
THE FINAL FATE OF STARS THAT IGNITE NEON AND OXYGEN OFF-CENTER: ELECTRON CAPTURE OR IRON CORE-COLLAPSE SUPERNOVA?
In the ONeMg cores of 8.8–9.5 M☉ stars, neon and oxygen burning is ignited off-center. Whether or not the neon-oxygen flame propagates to the center is critical for determining whether these stars
Electron-capture Supernovae of Super-AGB Stars: Sensitivity on Input Physics
Stars of M ∼ 8–10 M⊙ on their main sequence form strongly electron-degenerate oxygen–neon–magnesium (ONeMg) cores and become super–asymptotic giant branch stars. If such an ONeMg core grows to 1.38
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