The Compactness of Presupernova Stellar Cores

Sukhbold, Tuguldur; Woosley, S. E.

doi:10.1088/0004-637x/783/1/10

Cited by 272 publications

(454 citation statements)

References 48 publications

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“…7). The progenitor models of Sukhbold and Woosley (2014) (also in Sukhbold et al 2016) are used. As this figure shows, whatever the position at which compactness is defined, it correlates extremely well with envelope binding energy.…”

Section: Compactnessmentioning

confidence: 99%

Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

et al. 2018

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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

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Section: Compactnessmentioning

confidence: 99%

Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

et al. 2018

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“…N8.8 denotes an 8.8 M ONe-Mg-core progenitor from Nomoto (1984Nomoto ( , 1987, N20 a 20 M SN 1987A progenitor from Nomoto and Hashimoto (1988), z9.6 a 9.6 M zero-metallicity progenitor provided by A. Heger (2012, private communication), and all s-models are solar metallicity progenitors from Sukhbold and Woosley (2014), Woosley and Heger (2015b), . The progenitors with the smallest compactness values are classified as "Crab-like", the more compact iron-core progenitors as "SN1987A-like".…”

Section: Connection To Observationsmentioning

confidence: 99%

Neutrino-Driven Explosions

Janka

2017

Handbook of Supernovae

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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.

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“…Sukhbold & Woosley (2014) suggested that ξ measured just prior to collapse correlates with ξ at bounce. Hence, in this paper we evaluate ξ with the precollapse density structures.…”

Section: Stellar Evolution and Progenitor Structuresmentioning

confidence: 99%

Neutrino-driven explosions of ultra-stripped Type Ic supernovae generating binary neutron stars

Suwa

Yoshida

Shibata

et al. 2015

Mon. Not. R. Astron. Soc.

104

116

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We study explosion characteristics of ultra-stripped supernovae (SNe), which are candidates of SNe generating binary neutron stars (NSs). As a first step, we perform stellar evolutionary simulations of bare carbon-oxygen cores of mass from 1.45 to 2.0 M ⊙ until the iron cores become unstable and start collapsing. We then perform axisymmetric hydrodynamics simulations with spectral neutrino transport using these stellar evolution outcomes as initial conditions. All models exhibit successful explosions driven by neutrino heating. The diagnostic explosion energy, ejecta mass, Ni mass, and NS mass are typically ∼ 10 50 erg, ∼ 0.1M ⊙ , ∼ 0.01M ⊙ , and ≈ 1.3M ⊙ , which are compatible with observations of rapidly-evolving and luminous transient such as SN 2005ek. We also find that the ultra-stripped SN is a candidate for producing the secondary low-mass NS in the observed compact binary NSs like PSR J0737-3039.

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The Compactness of Presupernova Stellar Cores

Cited by 272 publications

References 48 publications

Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

Neutrino-Driven Explosions

Neutrino-driven explosions of ultra-stripped Type Ic supernovae generating binary neutron stars

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