The Supernova Channel of Super-AGB Stars

By A. Poelarends, Falk Herwig, N. Langer, Alexander Heger. 2007

241 citations recorded by the source corpus.

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☉. We perform calculations with three different stellar evolution codes to judge the robustness of our results. The mass range significantly depends on the treatment of semiconvective mixing and convective overshooting. To consider the effect of a large number of thermal pulses, as expected in SAGB stars, we construct synthetic SAGB models that are calibrated through stellar evolution simulations. The synthetic model enables us to compute the evolution of the main properties of SAGB stars from the onset of thermal pulses until the core reaches the Chandrasekhar mass or is uncovered by the stellar wind. Thereby, we differentiate the stellar initial mass ranges that produce ONe WDs from that leading to electron-capture SNe. The latter is found to be 9.0–9.25 M☉ for our fiducial model, implying that electron-capture SNe would constitute about 4% of all SNe in the local universe. The error in this determination due to uncertainties in the third dredge-up efficiency and AGB mass-loss rate could lead to about a doubling of the number of electron-capture SNe, which provides a firm upper limit to their contribution to all supernovae of ~20%.

Subfields: Astronomy and Astrophysics, Instrumentation

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THE EFFECT OF STARBURST METALLICITY ON BRIGHT X-RAY BINARY FORMATION PATHWAYS (2010, background): “This cutoff corresponds both to the first appearances of electron-capture supernovae (ECS) (Nomoto 1984; Poelarends et al. 2008) in our simulations as well as the last iron-core collapse SN.”
A NEW CLASS OF LUMINOUS TRANSIENTS AND A FIRST CENSUS OF THEIR MASSIVE STELLAR PROGENITORS (2008, methodology): “Here we follow the scenario detailed by Poelarends et al. (2008) (see also Nomoto 1984, 1987; Ritossa et al. 1996, Seiss 2006, 2007; as well as Chugai 1997; Wheeler et al. 1998; Woosley et al. 2002; Eldridge et al. 2007; Wanajo et al. 2009).”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “The result is an interesting production of trans-iron elements between Zn and Zr for the progenitor of Nomoto (1984, 1987); the production factors are consistent with current rate estimates for ECSNe of about 4% of all supernovae (Poelarends et al. 2008).”
Ultra-stripped supernovae: progenitors and fate (2015, background): “It has previously been demonstrated that the initial mass range for producing EC SNe is smaller in single stars (Poelarends et al. 2008) compared to binary stars in non-degenerate systems (Podsiadlowski et al. 2004).”
The effect of pair-instability mass loss on black-hole mergers (2016, methodology): “…is estimated based on a selection of hydrodynamical supernova models that are initiated with stellar models obtained with detailed evolutionary calculations (Woosley et al. 2002; Heger et al. 2003; Fryer 2006; Limongi & Chieffi 2006; Dessart et al. 2007; Poelarends et al. 2008; Young et al. 2009).”
COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY (2011, background): “However, we note that Poelarends et al. (2008) found that this result was highly sensitive to their prescriptions for mass loss and dredge-up.”
Discovery of the Dust-Enshrouded Progenitor of SN 2008S with Spitzer (2008, background): “Due to these similarities, we conclude that the progenitor of SN 2008S was likely a dust-enshrouded AGB (corecollapse produced from electron capture in the O-Ne-Mg core, e.g., Eldridge et al. 2007; Poelarends et al. 2008) or red supergiant like the ones observed in the LMC.”
THE AGE AND MASS OF THE α HERCULIS TRIPLE-STAR SYSTEM FROM A MESA GRID OF ROTATING STARS WITH 1.3 ⩽ M/M☉ ⩽ 8.0 (2013, background): “…evolutionary status: assuming a high mass, it could be a red supergiant or a super-AGB star and a progenitor of iron or electron-capture core-collapse supernova (Poelarends et al. 2008; Smartt 2009), while in the lower mass regime (M < 5 M⊙), the star would be located near the upper tip of the AGB.”
THE COMPACTNESS OF PRESUPERNOVA STELLAR CORES (2013, methodology): “For qr = 0.001, the 15, 16 and 17 M⊙ models closely resembled previous models calculated with KEPLER and other codes for stars with mass near 10 M⊙ (Nomoto 1987; Poelarends et al. 2008; Wanajo et al. 2009).”
Progenitors of Core-Collapse Supernovae (2009, background): “Weak explosions from electron capture SNe have been proposed (Kitaura, Janka, and Hillebrandt 2006) but these occur after 2nd dredge up when the progenitors would be SAGB stars and hence rather luminous, log L/L⊙≃ 10 5 (Eldridge and Tout 2004, Poelarends et al. 2008).”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, background): “…813 Santa Barbara St., Pasadena, CA, 91101 URL: http://obs.carnegiescience.edu/ 5 Hubble and Carnegie-Princeton Fellow 6 Alfred P. Sloan Fellow One possibility is the collapse of stars near the8M⊙ threshold via an electron capture trigger (Miyaji et al. 1980; Nomoto 1984; Poelarends et al. 2008).”
Production of dust by massive stars at high redshift (2011, background): “However, theoretical predictions from stellar evolution models (e.g., Heger et al, 2003; Eldridge and Tout, 2004; Poelarends et al, 2008) indicate a higher upper mass limit for II-P SNe: For solar metallicity it is ∼25 M⊙ and increases with decreasing metallicity.”
Origin of multiple stellar populations in globular clusters and their helium enrichment (2008, background): “Conversely, a supernova (SN) explosion ends the life of the star if mass loss during the SAGB phase is insufficient to prevent the core from growing in mass until it finally collapses (e.g. Nomoto 1984; Ritossa, Garcia-Berro & Iben 1996, 1999; Poelarends et al. 2008).”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “Subsequently, the O+Ne+Mg core becomes strongly degenerate, and the envelope becomes similar to that of super AGB stars (Eldridge & Tout 2004, Poelarends et al. 2008) with a thin He-burning shell that undergoes thermal pulses and s-process nucleosynthesis.”
Yields of AGB and SAGB models with chemistry of low- and high-metallicity globular clusters (2013, background): “Alternatively, they evolve as ONe white dwarfs (Poelarends et al. 2008).”
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…”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “This is in good agreement with the upper limit estimated from a recent study of stellar evolution (∼ 20%, Poelarends et al. 2008) as well as the estimate for the rate of SN 2008Slike transients (∼ 20−30%, Thompson et al. 2008).”
Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, background): “The fate of super-AGBs depends on the competition between mass loss and core growth (Poelarends et al. 2007; Siess 2007a): if mass loss wins, they evolve into massive O–Ne white dwarfs (Nomoto 1984); if the core reaches the Chandrasekhar mass, they evolve into electron capture supernovae (ecSNe),…”