The Supernova Channel of Super-AGB Stars

  title={The Supernova Channel of Super-AGB Stars},
  author={Arend J. T. Poelarends and Falk Herwig and Norbert Langer and Alexander Heger},
  journal={The Astrophysical Journal},
  pages={614 - 625}
We study the late evolution of solar metallicity stars in the transition region between white dwarf formation and core collapse. This includes the super-asymptotic giant branch (super-AGB, SAGB) stars, which ignite carbon burning and form an oxygen-neon (ONe) core. SAGB star cores may grow to the Chandrasekhar mass because of continued H- and He-shell burning, ending as core-collapse supernovae. From stellar evolution models we find that the initial mass range for SAGB evolution is 7.5–9.25 M… 

Final evolution of super-AGB stars and supernovae triggered by electron capture

Abstract Stars of 8–10 M⊙ form a strongly electron-degenerate oxygen–neon–magnesium core which is more massive than ∼1.1 M⊙, and become super-Asymptotic Giant Branch stars. The oxygen–neon–magnesium

Evolution of massive AGB stars - III. the thermally pulsing super-AGB phase

Aims. We present the first simulations of the full evolution of super-AGB stars through the entire thermally pulsing AGB phase. We analyse their structural and evolutionary properties and determine

The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars

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

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-AGB Stars and their Role as Electron Capture Supernova Progenitors

Abstract We review the lives, deaths and nucleosynthetic signatures of intermediate-mass stars in the range ≈6–12 M⊙, which form super-AGB stars near the end of their lives. The critical mass

The end of super AGB and massive AGB stars - I. The instabilities that determine the final mass of AGB stars

Context. The literature is rich in analysis and results related to thermally pulsing-asymptotic giant branch (TP-AGB) stars, but the problem of the instabilities that arise and cause the divergence


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


Evidence suggests that the direct progenitor stars of some core-collapse supernovae (CCSNe) are luminous blue variables (LBVs), perhaps including some Type II “superluminous supernovae” (SLSNe). We

The Formation and Evolution of ONe White Dwarfs: Prospects for Accretion Induced Collapse

Abstract I review our current understanding of the evolution of stars which experience carbon burning under conditions of partial electron degeneracy and ultimately become thermally pulsing “super”

Progenitors of Core-Collapse Supernovae

Abstract Massive stars have a strong impact on their surroundings, in particular when they produce a core-collapse supernova at the end of their evolution. In these proceedings, we review the general



Presupernova Evolution of Rotating Massive Stars. II. Evolution of the Surface Properties

We investigate the evolution of the surface properties of models for rotating massive stars, i.e., their luminosities, effective temperatures, surface rotational velocities, and surface abundances of

The evolution and explosion of massive stars

Like all true stars, massive stars are gravitationally confined thermonuclear reactors whose composition evolves as energy is lost to radiation and neutrinos. Unlike lower-mass stars (M≲8M⊙),

Evolution of Asymptotic Giant Branch Stars

▪ Abstract The current status of modeling the evolution and nucleosynthesis of asymptotic giant branch (AGB) stars is reviewed. The principles of AGB evolution have been investigated in recent years

Evolution of massive AGB stars: I.Carbon burning phase

We present new computations of the evolution of solar metallicity stars in the mass range $9 {-} 12$ $M_{\odot}$. This first paper of a series focuses on the propagation of the carbon burning flame

Presupernova Evolution of Rotating Massive Stars. I. Numerical Method and Evolution of the Internal Stellar Structure

The evolution of rotating stars with zero-age main-sequence (ZAMS) masses in the range 8-25 M☉ is followed through all stages of stable evolution. The initial angular momentum is chosen such that the

The r-Process in Supernova Explosions from the Collapse of O-Ne-Mg Cores

While the origin of r-process nuclei remains a long-standing mystery, recent spectroscopic studies of extremely metal poor stars in the Galactic halo strongly suggest that it is associated with

Presupernova models and supernovae

Present status of the theories for presupernova evolution and triggering mechanisms of supernova explosions are summarized and discussed from the standpoint of the theory of stellar structure and


We systematically examine how the presence in a binary affects the final core structure of a massive star and its consequences for the subsequent supernova explosion. Interactions with a companion

Circumstellar envelopes and Asymptotic Giant Branch stars

Summary. Red giants are sometimes surrounded by envelopes, the result of the ejection of stellar matter at a large rate ( $\dot M> 10^{-7}M_\odot$/yr) and at a low velocity (10 km/s). In this review

Evolution and Yields of Extremely Metal-poor Intermediate-Mass Stars

Intermediate-mass stellar evolution tracks from the main sequence to the tip of the AGB for five initial masses (2-6 M☉) and metallicity Z = 0.0001 have been computed. The detailed one-dimensional