NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS

By S. Wanajo, K. Nomoto, Hans-Thomas Janka, Francisco-Shu Kitaura, Bernhard Müller. 2008

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We examine nucleosynthesis in the electron capture supernovae of progenitor asymptotic giant branch stars with an O–Ne–Mg core (with the initial stellar mass of 8.8 M☉). Thermodynamic trajectories for the first 810 ms after core bounce are taken from a recent state-of-the-art hydrodynamic simulation. The presented nucleosynthesis results are characterized by a number of distinct features that are not shared with those of other supernovae from the collapse of stars with iron core (with initial stellar masses of more than 10 M☉). First is the small amount of 56Ni (0.002–0.004 M☉) in the ejecta, which can be an explanation for the observed properties of faint supernovae such as SNe 2008S and 1997D. In addition, the large Ni/Fe ratio is in reasonable agreement with the spectroscopic result of the Crab nebula (the relic of SN 1054). Second is the large production of 64Zn, 70Ge, light p-nuclei (74Se, 78Kr, 84Sr, and 92Mo), and in particular, 90Zr, which originates from the low Ye (0.46–0.49, the number of electrons per nucleon) ejecta. We find, however, that only a 1%–2% increase of the minimum Ye moderates the overproduction of 90Zr. In contrast, the production of 64Zn is fairly robust against a small variation of Ye. This provides the upper limit of the occurrence of this type of events to be about 30% of all core-collapse supernovae.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6b9912c9a072931dbc967acf256ee35c228d5513

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Citations in the corpus

THE REMARKABLE DEATHS OF 9–11 SOLAR MASS STARS (2015, methodology): “Because of the low mass of the ejecta, the small abundances of heavy elements, and the presence of a pulsar, this supernova has often been associated with the death of a star that, on the main sequence, had a mass ∼ 10M⊙ (Nomoto et al. 1982; Wanajo et al. 2009).”
Production of dust by massive stars at high redshift (2011, unknown): “According to Wanajo et al (2009), about 30 % of all CCSNe couldappear as ECSNe if all stars in the mass range of 8–10 M⊙ end in the explosion channel.”
Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, background): “This led to considerable study of this mass range, in particular to detailed modelling of EC-SNe (e.g Ning et al. 2007; Wanajo et al. 2003, 2009; Qian & Wasserburg 2003, 2007).”
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).”
ELECTRON-CAPTURE SUPERNOVAE AS THE ORIGIN OF ELEMENTS BEYOND IRON (2010, methodology): “Wanajo et al. (2009) further speculated that the nucleosynthetic outcome could be considerably altered in the 1 Technische Universität München, Excellence Cluster Universe, Boltzmannstr.”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, methodology): “Nucleosynthesis calculations based on modern, spherically symmetric ECSN models were first performed by Hoffman et al. (2008) and Wanajo et al. (2009).”
SN 2008S: An electron-capture SN from a super-AGB progenitor? (2009, background): “…Chandrasekhar mass, high pressure and density lead to electron capture onto24Mg and 20Ne, the electron degeneracy pressure decreases and the core may collapse beforan iron core is formed (Miyaji et al. 1980; Miyaji & Nomoto 1987; Hashimoto et al. 1993; Poelarends et al. 2008; Wanajo et al. 2008).”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, background): “9M⊙), called the O-Ne-Mg or electron capture supernova (e.g., Kitaura et al. 2006; Janka et al. 2008; Wanajo et al. 2009, 2011).”
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).”