Core-Collapse Supernovae From 9 to 120 Solar Masses Based on Neutrino-Powered Explosions

Sukhbold, Tuguldur; Ertl, Thomas; Woosley, S. E.; Brown, Justin M.; Janka, Hans‐Thomas

doi:10.3847/0004-637x/821/1/38

Cited by 1,112 publications

(1,730 citation statements)

References 133 publications

(384 reference statements)

Supporting

112

Mentioning

1,591

Contrasting

Unclassified

Order By: Relevance

“…As previously stated, for most of the relevant mass function, the envelope binding energy exterior to a given interior mass is an increasing function of progenitor mass. It is this "barrier" that may set the limit to the range of massive stars that can explode and leave behind neutron stars, although it cannot be excluded that the progenitor mass range that yields neutron stars, and not black holes, may be discontinuous (Sukhbold et al 2016). Figure 7 portrays various exterior binding energies and Fig.…”

Section: Compactnessmentioning

confidence: 99%

Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

et al. 2018

View full text Add to dashboard Cite

We explore with self-consistent 2D FORNAX simulations the dependence of the outcome of collapse on many-body corrections to neutrino-nucleon cross sections, the nucleon-nucleon bremsstrahlung rate, electron capture on heavy nuclei, pre-collapse seed perturbations, and inelastic neutrino-electron and neutrino-nucleon scattering. Importantly, proximity to criticality amplifies the role of even small changes in the neutrino-matter couplings, and such changes can together add to produce outsized effects. When close to the critical condition the cumulative result of a few small effects (including seeds) that individually have only modest consequence can convert an anemic into a robust explosion, or even a dud into a blast. Such sensitivity is not seen in one dimension and may explain the apparent heterogeneity in the outcomes of detailed simulations performed internationally. A natural conclusion is that the different groups collectively are closer to a realistic understanding of the mechanism of core-collapse supernovae than might have seemed apparent. Supernovae Edited by

show abstract

Section: Compactnessmentioning

confidence: 99%

Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

et al. 2018

View full text Add to dashboard Cite

show abstract

“…Accordingly, since WW95, there have been updates in the nucleosynthesis models of massive stars Nomoto et al 2013;West et al 2016). Recently, Sukhbold et al (2016) presented yields with models where the explosion energies were predicted rather than assumed. According to the authors, the yields on Mg and Al are still slightly deficient, possibly due to a low CO core-size, which in turn may be a consequence of neglecting rotation or differences in overshooting mixing.…”

Section: Comparison With Literature Oxygen Abundancesmentioning

confidence: 99%

Tracing the evolution of the Galactic bulge with chemodynamical modelling of alpha-elements

Friaça

Barbuy

2017

A&A

View full text Add to dashboard Cite

Context. Galactic bulge abundances can be best understood as indicators of bulge formation and nucleosynthesis processes by comparing them with chemo-dynamical evolution models. Aims. The aim of this work is to study the abundances of alpha-elements in the Galactic bulge, including a revision of the oxygen abundance in a sample of 56 bulge red giants. Methods. Literature abundances for O, Mg, Si, Ca and Ti in Galactic bulge stars are compared with chemical evolution models. For oxygen in particular, we reanalysed high-resolution spectra obtained using FLAMES+UVES on the Very Large Telescope, now taking each star's carbon abundances, derived from CI and C 2 lines, into account simultaneously.Results. We present a chemical evolution model of alpha-element enrichment in a massive spheroid that represents a typical classical bulge evolution. The code includes multi-zone chemical evolution coupled with hydrodynamics of the gas. Comparisons between the model predictions and the abundance data suggest a typical bulge formation timescale of 1-2 Gyr. The main constraint on the bulge evolution is provided by the O data from analyses that have taken the C abundance and dissociative equilibrium into account. Mg, Si, Ca and Ti trends are well reproduced, whereas the level of overabundance critically depends on the adopted nucleosynthesis prescriptions.

show abstract

“…(Figure courtesy of Thomas Ertl) Fig. 13 Explosion and remnant properties as functions of progenitor ZAMS mass for the compilation of single-star, solar-metallicity progenitor models considered by Sukhbold et al (2016). The results are based on 1D simulations with a calibrated neutrino "engine" (for more details, see Ertl et al, 2016;Sukhbold et al, 2016).…”

Section: Progenitor-explosion-remnant Connectionmentioning

confidence: 99%

Neutrino-Driven Explosions

Janka

2017

Handbook of Supernovae

View full text Add to dashboard Cite

The question why and how core-collapse supernovae (SNe) explode is one of the central and most long-standing riddles of stellar astrophysics. Solving this problem is crucial for deciphering the SN phenomenon, for predicting its observable signals such as light curves and spectra, nucleosynthesis yields, neutrinos, and gravitational waves, for defining the role of SNe in the dynamical and chemo-dynamical evolution of galaxies, and for explaining the birth conditions and properties of neutron stars (NSs) and stellar-mass black holes. Since the formation of such compact remnants releases over hundred times more energy in neutrinos than the kinetic energy of the SN explosion, neutrinos can be the decisive agents for powering the SN outburst. According to the standard paradigm of the neutrino-driven mechanism, the energy transfer by the intense neutrino flux to the medium behind the stagnating core-bounce shock, assisted by violent hydrodynamic mass motions (sometimes subsumed by the term "turbulence"), revives the outward shock motion and thus initiates the SN explosion. Because of the weak coupling of neutrinos in the region of this energy deposition, detailed, multi-dimensional hydrodynamic models including neutrino transport and a wide variety of physics are needed to assess the viability of the mechanism. Owing to advanced numerical codes and increasing supercomputer power, considerable progress has been achieved in our understanding of the physical processes that have to act in concert for the success of neutrino-driven explosions. First studies begin to reveal observational implications and avenues to test the theoretical picture by data from individual SNe and SN remnants but also from population-integrated observables. While models will be further refined, a real breakthrough is expected through the next Galactic core-collapse SN, when neutrinos and gravitational waves can be used to probe the conditions deep inside the dying star.

show abstract

Core-Collapse Supernovae From 9 to 120 Solar Masses Based on Neutrino-Powered Explosions

Cited by 1,112 publications

References 133 publications

Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

Tracing the evolution of the Galactic bulge with chemodynamical modelling of alpha-elements

Neutrino-Driven Explosions

Contact Info

Product

Resources

About