PROGENITOR-EXPLOSION CONNECTION AND REMNANT BIRTH MASSES FOR NEUTRINO-DRIVEN SUPERNOVAE OF IRON-CORE PROGENITORS

By Marcella Ugliano, Hans-Thomas Janka, Andreas Marek, A. Arcones. 2012

315 citations recorded by the source corpus.

We perform hydrodynamic supernova (SN) simulations in spherical symmetry for over 100 single stars of solar metallicity to explore the progenitor-explosion and progenitor-remnant connections established by the neutrino-driven mechanism. We use an approximative treatment of neutrino transport and replace the high-density interior of the neutron star (NS) by an inner boundary condition based on an analytic proto-NS core-cooling model, whose free parameters are chosen such that explosion energy, nickel production, and energy release by the compact remnant of progenitors around 20 M☉ are compatible with SN 1987A. Thus, we are able to simulate the accretion phase, initiation of the explosion, subsequent neutrino-driven wind phase for 15–20 s, and the further evolution of the blast wave for hours to days until fallback is completed. Our results challenge long-standing paradigms. We find that remnant mass, launch time, and properties of the explosion depend strongly on the stellar structure and exhibit large variability even in narrow intervals of the progenitors’ zero-age main-sequence mass. While all progenitors with masses below ∼15 M☉ yield NSs, black hole (BH) as well as NS formation is possible for more massive stars, where partial loss of the hydrogen envelope leads to weak reverse shocks and weak fallback. Our NS baryonic masses of ∼1.2–2.0 M☉ and BH masses >6 M☉ are compatible with a possible lack of low-mass BHs in the empirical distribution. Neutrino heating accounts for SN energies between some 1050 erg and ∼2 × 1051 erg but can hardly explain more energetic explosions and nickel masses higher than 0.1–0.2 M☉. These seem to require an alternative SN mechanism.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5072306ef60e20c76132500d3c59f0c14a905da1

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Citations in the corpus

Colloquium: Perspectives on core-collapse supernova theory (2012, background): “More massive stars are more difficult to explode and at some point probably make black holes (Ugliano et al. 2012; O’Connor & Ott 2011; Fryer et al. 1999).”
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…”
THE ROLE OF TURBULENCE IN NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2014, background): “Such a star, if it were to occur in Nature, would be likely to result in a success- ful explosion and the formation of a neutron star based on both its compactness (O’Connor & Ott 2011; Ugliano et al. 2012; Kochanek 2014) and its low helium core mass (Clausen et al. 2014).”
Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, background): “We are aware that many detailed studies of SN explosions and their progenitors find evidence for a nonmonotonic mapping of (ZAMS) progenitor star mass and final compact object mass (Ugliano et al. 2012; Pejcha & Thompson 2015), which is not included here.”
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].”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, background): “…deviations in progenitor internal structure that have been seen to affect the outcomes of parameterized 1D simulations of the same 101 progenitors (Ugliano et al. 2012), and core compactness is not an observable parameter that can be translated into observational comparisons like those in Figure…”
Pulsational Pair-instability Supernovae (2016, background): “23 Wilson et al. 1986; Fryer 1999; Fryer & Kalogera 2001; Ugliano et al. 2012; Pejcha & Thompson 2015).”
A simple approach to the supernova progenitor–explosion connection (2016, methodology): “, and possibly a third one at 1.9 M which is qualitatively similar to Zhang, Woosley & Heger (2008) and case a) of Pejcha & Thompson (2015), but more conspicuous than in the work of Ugliano et al. (2012).”
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, methodology): “Neutrino transport and neutrino-matter interactions were treated by the ray-by-ray gray neutrino transport scheme of Scheck et al. (2006) including a slight modification of the prescription for neutrino mean energies at the inner grid boundary (Ugliano et al. 2012).”
THE COMPACTNESS OF PRESUPERNOVA STELLAR CORES (2013, background): “…between this structure and the likelihood of explosion has been noted many times (Burrows & Lattimer 1987; Fryer 1999; O’Connor & Ott 2011; Ugliano et al. 2012), but little attention has been given to explaining just why the compactness has the values that it does, or why different…”
VERY LOW ENERGY SUPERNOVAE FROM NEUTRINO MASS LOSS (2013, background): “Black holes are expected to form in a significant fraction of massive star deaths (e.g., O’Connor & Ott 2011; Ugliano et al. 2012) and it seems possible that in at least some of these cases the black hole will form without generating an outgoing shock.”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, background): “In order to leave behind a slowly cooling neutron star and not a black hole, shock revival must occur within a few hundred milliseconds of bounce (O’Connor & Ott 2011; Ugliano et al. 2012).”
Merging black hole binaries with the SEVN code (2018, background): “…al. 2015 for a recent review), several studies (Fryer 1999; Fryer, Woosley & Heger 2001; Heger et al. 2003; O’Connor & Ott 2011; Fryer et al. 2012; Ugliano et al. 2012; Ertl et al. 2016) suggest that if the mass and/or the compactness of the star at the onset of collapse are sufficiently large,…”
MISSING BLACK HOLES UNVEIL THE SUPERNOVA EXPLOSION MECHANISM (2011, background): “Second, the predicted by Ugliano et al. (2012) mass gap starts over 6 M⊙ which again is in clear contradiction with mass measurement of some black holes with masses below that value (e.g., ∼ 5.1 M⊙ for a black hole in XTE J1650-500; Slany & Stuchlik 2008).”
The mass spectrum of compact remnants from the parsec stellar evolution tracks (2015, methodology): “24 shows that there is a signiﬁcant mass gap between the heaviest NS ( ∼ 2M (cid:4) ) and the lightest BH ( ∼ 12M (cid:4) ), quite larger than the observed one ( ¨Ozel et al. 2010; Farr et al. 2011; Ugliano et al. 2012; Kochanek 2014; Neustroev et al. 2014).”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, methodology): “The mean neutrino energies of the neutrino fluxes entering the grid are prescribed as functions of the temperature in the first radial cell of the computational grid as described by Ugliano et al. (2012).”
Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars (2015, methodology): “…explosions has reinvigorated the study of the explodability of stars and in particular, three independent analyses by O’Connor & Ott (2011), Ugliano et al. (2012), and Sukhbold & Woosley (2014) and have used the compactness parameter (defined in O’Connor & Ott) which quantifies the core…”