THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS

By O. Pejcha, T. Thompson. 2014

152 citations recorded by the source corpus.

If the neutrino luminosity from the proto-neutron star formed during a massive star core collapse exceeds a critical threshold, a supernova (SN) results. Using spherical quasi-static evolutionary sequences for hundreds of progenitors over a range of metallicities, we study how the explosion threshold maps onto observables, including the fraction of successful explosions, the neutron star (NS) and black hole (BH) mass functions, the explosion energies (ESN) and nickel yields (MNi), and their mutual correlations. Successful explosions are intertwined with failures in a complex pattern that is not simply related to initial progenitor mass or compactness. We predict that progenitors with initial masses of 15 ± 1, 19 ± 1, and ∼21–26 M☉ are most likely to form BHs, that the BH formation probability is non-zero at solar-metallicity and increases significantly at low metallicity, and that low luminosity, low Ni-yield SNe come from progenitors close to success/failure interfaces. We qualitatively reproduce the observed ESN–MNi correlation, we predict a correlation between the mean and width of the NS mass and ESN distributions, and that the means of the NS and BH mass distributions are correlated. We show that the observed mean NS mass of ≃ 1.33 M☉ implies that the successful explosion fraction is higher than 0.35. Overall, we show that the neutrino mechanism can in principle explain the observed properties of SNe and their compact objects. We argue that the rugged landscape of progenitors and outcomes mandates that SN theory should focus on reproducing the wide ranging distributions of observed SN properties.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3ae5901d45628562970ab1c91a2f365125d9e5ff

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Citations in the corpus

A High-resolution Study of Presupernova Core Structure (2017, background): “…albeit approximately, whether a star with a given mass blows up or collapses to a black hole simply from looking at one-dimensional models for stellar evolution (O’Connor & Ott 2011, 2013; Ugliano et al. 2012; Pejcha & Thompson 2015; Ertl et al. 2016; Sukhbold et al. 2016; Müller et al. 2016).”
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…”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, background): “…symmetric (1D) hydrodynamic simulations, but their basic findings were confirmed by other groups working with semi-analytic descriptions in 1D (Pejcha & Thompson 2015) and approximate neutrino transport in two- and three-dimensional (2D, 1 Max-Planck-Institut für Astrophysik,…”
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.”
CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, background): “A similar correlation between 56Ni and kinetic energy has been discussed by Pejcha & Thompson (2015) and compared with observational data (their Figure 20).”
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].”
A simple approach to the supernova progenitor–explosion connection (2016, methodology): “For these purposes, parametrized 1D simulations are not a viable option even if they are only used to provide time-dependent input data for an analytic model as in Pejcha & Thompson (2015).”
Measuring the Progenitor Masses and Dense Circumstellar Material of Type II Supernovae (2017, methodology): “This correlation has previously been seen in nucleosynthetic simulations (Sukhbold et al. 2016) and light-curve parameterization methods (Pejcha & Thompson 2015).”
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).”
MERGING BLACK HOLE BINARIES IN GALACTIC NUCLEI: IMPLICATIONS FOR ADVANCED-LIGO DETECTIONS (2016, background): “Recent theoretical studies suggest that the birth kicks may not be directly correlated with the BH mass (Repetto & Nelemans 2015; Pejcha & Thompson 2015), and that the distribution of black hole kick velocities could be similar to that of neutron stars σnatal ≈ 200 km s−1 (but see Mandel 2016).”
Pulsational Pair-instability Supernovae (2016, background): “23 Wilson et al. 1986; Fryer 1999; Fryer & Kalogera 2001; Ugliano et al. 2012; Pejcha & Thompson 2015).”
A new route towards merging massive black holes (2016, background): “…physics of the evolution of massive stars, although there are still significant uncertainties, for instance, in the treatment of stellar winds (Langer 2012), rotational mixing (Maeder & Meynet 2012), and the BH formation itself (Heger et al. 2003; Ugliano et al. 2012; Pejcha & Thompson 2015).”