ELECTRON-CAPTURE SUPERNOVAE AS THE ORIGIN OF ELEMENTS BEYOND IRON

By S. Wanajo, Hans-Thomas Janka, B. Mueller. 2010

191 citations recorded by the source corpus.

We examine electron-capture supernovae (ECSNe) as sources of elements heavier than iron in the solar system and in Galactic halo stars. Nucleosynthesis calculations are performed on the basis of thermodynamic histories of mass elements from a fully self-consistent, two-dimensional hydrodynamic explosion model of an ECSN. We find that neutron-rich convective lumps with an electron fraction down to Ye,min = 0.40, which are absent in the one-dimensional counterpart, allow for interesting production of elements between the iron group and N = 50 nuclei (from Zn to Zr, with little Ga) in nuclear (quasi-)equilibrium. Our models yield very good agreement with the Ge, Sr, Y, and Zr abundances of r-process-deficient Galactic halo stars and constrain the occurrence of ECSNe to ∼4% of all stellar core-collapse events. If tiny amounts of additional material with slightly lower Ye,min down to ∼0.30–0.35 were also ejected—which presently cannot be excluded because of the limitations of resolution and two dimensionality of the model—a weak r-process can yield elements beyond N = 50 up to Pd, Ag, and Cd as observed in the r-process-deficient stars.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c2c9b03af05f0ca57fc9e50a16f72035a5dfd6a1

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Citations in the corpus

MAGNETOROTATIONALLY DRIVEN SUPERNOVAE AS THE ORIGIN OF EARLY GALAXY r-PROCESS ELEMENTS? (2012, background): “Electron-capture supernovae, which explode without a long phase of accretion onto the proto-neutron star (PNS), apparently provide more favorable conditions (Wanajo et al. 2011).”
Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, background): “…site (e.g Hoffman et al. 2008) the frequency of EC-SNe is still of interest as they may contribute to the weak rprocess component (Hansen et al. 2012) as well as be important contributors to the galactic inventory of a range of isotopes such as 48Ca and 60Fe (Wanajo et al. 2011, 2013a,b).”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, background): “We speculate that the O–Ne–Mg core explosion of Wanajo et al. (2011), where convective overturn but not SASI played a role, may be a case where we have encountered consequences of the dipolar leptonemission asymmetry in a 2D model.”
PRODUCTION OF ALL THE r-PROCESS NUCLIDES IN THE DYNAMICAL EJECTA OF NEUTRON STAR MERGERS (2014, background): “Nucleosynthesis studies with such physical environments confirm that CCSNe produce elements only up to the atomic mass number A ∼ 110 (Wanajo et al. 2011; Wanajo 2013).”
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).”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, unknown): “1 in Wanajo et al. 2011).”
Astrophysics with Extraterrestrial Materials (2016, background): “…site or sites where it occurs remain unknown, though neutrino winds from SNe, low-mass SNe, mergers of neutron stars with each other or with black holes, and magnetorotationally driven SNe have all been suggested (Meyer 1994, Freiburghaus et al. 1999, Wanajo et al. 2011, Winteler et al. 2012).”
Origin of the heaviest elements: The rapid neutron-capture process (2019, background): “However, despite all remaining uncertainties in the explosion mechanism, recent conclusions are that at most a weak r-process can occur under these conditions (Wanajo et al., 2011; Mart́ınez-Pinedo et al., 2012; Roberts et al., 2012; Curtis et al., 2019), because weak interactions with electron neut”
r-PROCESS NUCLEOSYNTHESIS IN DYNAMICALLY EJECTED MATTER OF NEUTRON STAR MERGERS (2011, methodology): “…extreme sensitivity to the detailed conditions in the ejecta, whose viability for strong r-processing could not be verified by sophisticated hydrodynamical models (e.g., Hoffman et al. 2008; Janka et al. 2008; Roberts et al. 2010; Hüdepohl et al. 2010; Fischer et al. 2010; Wanajo et al. 2011).”
CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, methodology): “The computed properties of this explosion (energy around 0.1 B and 56Ni mass below 0.01 M ; see following section) turn out to be fully consistent with the observational limits for Crab.”
SYSTEMATICS OF DYNAMICAL MASS EJECTION, NUCLEOSYNTHESIS, AND RADIOACTIVELY POWERED ELECTROMAGNETIC SIGNALS FROM NEUTRON-STAR MERGERS (2013, background): “…may well be a major source of r-process elements and current supernova models cannot provide suitable conditions for the formation of the heaviest r-process elements (Hoffman et al. 2008; Janka et al. 2008; Roberts et al. 2010; Hüdepohl et al. 2010; Fischer et al. 2010; Wanajo et al. 2011).”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, methodology): “…luminosities and mean energies and to the ejection velocity of the convective plumes (which may be different in 3D compared to 2D, or exhibit stochastic variations), Wanajo et al. (2011) also explored the effect of potential uncertainties in the minimum Ye in the ejecta on the nucleosynthesis.”