CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS

By T. Sukhbold, T. Ertl, Stan Woosley, Justin M. Brown, Hans-Thomas Janka. 2015

562 citations recorded by the source corpus.

Nucleosynthesis, light curves, explosion energies, and remnant masses are calculated for a grid of supernovae (SNe) resulting from massive stars with solar metallicity and masses from 9.0 to 120 M ⊙ . The full evolution is followed using an adaptive reaction network of up to 2000 nuclei. A novel aspect of the survey is the use of a one-dimensional neutrino transport model for the explosion. This explosion model has been calibrated to give the observed energy for SN 1987A, using five standard progenitors, and for the Crab SN using a 9.6 M ⊙ progenitor. As a result of using a calibrated central engine, the final kinetic energy of the SN is variable and sensitive to the structure of each pre-SN star. Many progenitors with extended core structures do not explode, but become black holes (BHs), and the masses of exploding stars do not form a simply connected set. The resulting nucleosynthesis agrees reasonably well with the Sun provided that a reasonable contribution from SNe Ia is also allowed, but with a deficiency of light s-process isotopes. The resulting neutron star initial mass function has a mean gravitational mass near 1.4 M ⊙ . The average BH mass is about 9 M ⊙ if only the helium core implodes, and 14 M ⊙ if the entire pre-SN star collapses. Only ∼10% of SNe come from stars over 20 M ⊙ , and some of these are Type Ib or Ic. Some useful systematics of Type IIp light curves are explored.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/da36d4e6587a81c7671b9b343e0931499ae86668

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Citations in the corpus

Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “We consider seven stellar evolution progenitors from Sukhbold et al. (2016) with ZAMS masses of 9Me, 10Me, 11Me, 12Me, 13Me, 19Me, and 60Me.”
Forming short-period Wolf–Rayet X-ray binaries and double black holes through stable mass transfer (2017, background): “…mass-loss of both stars, and by assuming that at the end of the life of the Wolf-Rayet star as a WC-type star, 90% of the mass of the WC star disappeared into the black hole (cf. Heger 2012; Sukhbold et al. 2016), meaning that just only the gravitational binding energy of the helium star is lost.”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “In our models, the radii at the density 1011 g cm−3 are nearly the same as the radii at the density 1010 g cm−3. genitor ZAMS mass is not monotonic (Sukhbold et al. 2016) and, moreover, may be intrinsically chaotic (Sukhbold et al. 2017).”
What can be learned from a future supernova neutrino detection (2017, background): “Various authors have confirmed this prediction, sometimes refining / replacing the criteria for explodability by replacing compactness with another quantity which measures something similar [166, 156, 167, 164, 168, 169].”
Pulsational Pair-instability Supernovae (2016, background): “Additional description of the code physics is given in Woosley & Heger (2007) and Sukhbold et al. (2016).”
The spin of the second-born black hole in coalescing binary black holes (2018, background): “Stellar-mass black holes (BHs) are formed from the gravitational collapse of massive stars (&20 M ; e.g., Fryer 1999; Heger et al. 2003; Sukhbold et al. 2016) after they exhaust the nuclear fuel at their centers.”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “…gravitational tug-boat mechanism would mean that BH formation events with significant SN fallback are rare in the Galactic neighborhood, compatible with conclusions drawn from recent theoretical studies of the progenitor-SN connection (Ugliano et al. 2012; Ertl et al. 2016; Sukhbold et al. 2016).”
Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “…& Prieto (2015) found that the kinetic energy of the ejecta in a sample of Type IIP supernovae never exceeds 3 foes while on the theoretical one Sukhbold et al. (2016), O’Connor & Ott (2011) and Ertl et al. (2016) find that stellar models more massive than 25 − 30 M fail to explode (even if…”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, unknown): “More phenomenological models (Ugliano et al. 2012; Ertl et al. 2016; Pejcha & Thompson 2015; Müller et al. 2016a; Sukhbold et al. 2016) are presently the only viable theoretical approach for this purpose, but it is imperative that they be put on a firmer footing with the help of select…”
Measuring the Progenitor Masses and Dense Circumstellar Material of Type II Supernovae (2017, methodology): “From the large set of progenitor models presented in Sukhbold et al. (2016), we choose a subset of models in the mass range between 9 and 25Me in steps of 0.5Me.”
A High-resolution Study of Presupernova Core Structure (2017, methodology): “For just the limited mass range 12 - 27 M , the average black hole masses from Sukhbold et al. (2016) were previously 6.52 and 15.3 M respectively for the helium core and full star assumptions.”
A simple approach to the supernova progenitor–explosion connection (2016, methodology): “The input physics is very similar to the models of Sukhbold & Woosley (2014) and Sukhbold et al. (2016), except for updates in the neutrino loss rates (Itoh et al. 1996) and the initial solar composition (Asplund et al. 2009).”
BPASS predictions for binary black hole mergers (2016, background): “However at higher initial masses, mass-loss can still lead to the formation of neutron stars (e.g. Eldridge & Tout 2004; Heger et al. 2003; Ugliano et al. 2012; Sukhbold et al. 2016).”
The search for failed supernovae with the Large Binocular Telescope: confirmation of a disappearing star (2016, background): “…et al. 2009; Smartt 2015) and corresponds to a progenitor with a high “compactness” parameter that is considered most likely to result in a failed supernova (O’Connor & Ott 2011; Ugliano et al. 2012; Horiuchi et al. 2014; Sukhbold & Woosley 2014; Pejcha & Thompson 2015; Sukhbold et al. 2016).”
Revisiting Supernova 1987A constraints on dark photons (2016, result): “Two new elements in our calculation, compared to previous work, are that (2)In fact, a neutrino burst that sustains an explosive front compatible with the observed energetics is challenging [39, 40] (though not impossible [41, 42]) to obtain in numerical simulations, and it is possible that the expl”