Black Hole Formation in Failing Core-Collapse Supernovae

O’Connor, Evan; Ott, Christian D.

doi:10.1088/0004-637x/730/2/70

Cited by 713 publications

(684 citation statements)

References 94 publications

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“…By replacing the proto-neutron star (PNS) interior with an inner boundary condition, they followed an unprecedentedly long-term evolution over hours to days after bounce in spherical symmetry. Their results also lent support to the finding by O'Connor & Ott (2011) that the compactness parameter is a good measure to diagnose the progenitor-explosion and the progenitor-remnant correlation (see also Pejcha & Thompson 2014;Perego et al 2015).…”

Section: Introductionsupporting

confidence: 70%

“…Here it should be noted that the above threshold is for a cold NS, whereas the PNS soon after bounce is still hot. At this phase, the contribution of thermal pressure to the maximum mass cannot be neglected, so that the maximum mass of the hot PNS is bigger than that of the cold NS (O'Connor & Ott 2011;Hempel et al 2012). Based on a systematic 1D GR simulation with approximate neutrino transport, O'Connor & Ott (2011) showed that the maximum gravitational mass of the hot PNSs, which is bigger for models with high compactness, ranges from 2.1M ⊙ (ξ 2.5,cb = 0.20) 2 to 2.5 M ⊙ (1.15).…”

Section: Resultsmentioning

confidence: 99%

“…By performing general-relativistic (GR) 1.5D simulations for over 100 presupernova models using a leakage scheme, O'Connor & Ott (2011) were the first to point out that the postbounce dynamics and the progenitorremnant connections are predictable basically by a single parameter, compactness of the stellar core at bounce (see also O'Connor & Ott 2013). Along this line, Ugliano et al (2012) performed 1D hydrodynamic simulations for 101 progenitors of Woosley et al (2002).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Systematic features of axisymmetric neutrino-driven core-collapse supernova models in multiple progenitors

Nakamura

Takiwaki

Kuroda

et al. 2015

Publications of the Astronomical Society of Japan

127

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We present an overview of two-dimensional (2D) core-collapse supernova simulations employing neutrino transport scheme by the isotropic diffusion source approximation. We study 101 solar-metallicity, 247 ultra metal-poor, and 30 zero-metal progenitors covering zero-age main sequence mass from 10.8 M ⊙ to 75.0 M ⊙ . Using the 378 progenitors in total, we systematically investigate how the differences in the structures of these multiple progenitors impact the hydrodynamics evolution. By following a long-term evolution over 1.0 s after bounce, most of the computed models exhibit neutrino-driven revival of the stalled bounce shock at ∼ 200 -800 ms postbounce, leading to the possibility of explosion. Pushing the boundaries of expectations in previous one-dimensional (1D) studies, our results confirm that the compactness parameter ξ that characterizes the structure of the progenitors is also a key in 2D to diagnose the properties of neutrinodriven explosions. Models with high ξ undergo high ram pressure from the accreting matter onto the stalled shock, which affects the subsequent evolution of the shock expansion and the mass of the protoneutron star under the influence of neutrino-driven convection and the standing accretion-shock instability. We show that the accretion luminosity becomes higher for models with high ξ, which makes the growth rate of the diagnostic explosion energy higher and the synthesized nickel mass bigger. We find that these explosion characteristics tend to show a monotonic increase as a function of the compactness parameter ξ.

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Section: Introductionsupporting

confidence: 70%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Systematic features of axisymmetric neutrino-driven core-collapse supernova models in multiple progenitors

Nakamura

Takiwaki

Kuroda

et al. 2015

Publications of the Astronomical Society of Japan

127

View full text Add to dashboard Cite

show abstract

“…The latter prescription is under the assumption that the BH formation is controlled by the compactness of the stellar core at the time of collapse: low compactness stars are more likely to explode as SNe and produce NSs, while high-compactness stars are more likely to evolve to failed SNe that produce BHs (O'Connor & Ott 2011). In this case we assume MBH = MHe or MCO, where MHe is the He core masses prior to core collapse (e.g., Smith et al 2011;Smith & Arnett 2014;Shiode & Quataert 2014;Sukhbold & Woosley 2014;Clausen et al 2015;Kochanek 2014Kochanek , 2015.…”

Section: Remnant Massmentioning

confidence: 99%

On the formation of galactic black hole low-mass X-ray binaries

Wang

Jia

2016

Mon. Not. R. Astron. Soc.

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Currently, there are 24 black hole (BH) X-ray binary systems that have been dynamically confirmed in the Galaxy. Most of them are low-mass X-ray binaries (LMXBs) comprised of a stellar-mass BH and a low-mass donor star. Although the formation of these systems has been extensively investigated, some crucial issues remain unresolved. The most noticeable one is that, the low-mass companion has difficulties in ejecting the tightly bound envelope of the massive primary during the spiral-in process. While initially intermediate-mass binaries are more likely to survive the common envelope (CE) evolution, the resultant BH LMXBs mismatch the observations. In this paper, we use both stellar evolution and binary population synthesis to study the evolutionary history of BH LMXBs. We test various assumptions and prescriptions for the supernova mechanisms that produce BHs, the binding energy parameter, the CE efficiency, and the initial mass distributions of the companion stars. We obtain the birthrate and the distributions of the donor mass, effective temperature and orbital period for the BH LMXBs in each case. By comparing the calculated results with the observations, we put useful constraints on the aforementioned parameters. In particular, we show that it is possible to form BH LMXBs with the standard CE scenario if most BHs are born through failed supernovae.

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“…The delayed neutrino-heating model for CCSNe posits that a small fraction of the neutrinos emitted from near the protoneutron star are absorbed near the stalled shock, thereby depositing enough energy to reinvigorate the shock's outward progress. This shock revival must occur within a few hundreds of milliseconds to ∼1-2 s of core bounce to avoid black hole formation or a top-heavy neutron star mass distribution (O'Connor & Ott 2011). Since the neutrino mechanism strongly depends on how efficiently energy is transported by neutrinos from near the protoneutron star to the region just behind the shock and on how this energy deposition affects the hydrodynamic evolution near the shock, an accurate treatment of hydrodynamics and non-equilibrium neutrino transport is a key requirement for simulating CCSNe.…”

Section: Introductionmentioning

confidence: 99%

General-Relativistic Three-Dimensional Multi-Group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae

Roberts

Ott

Haas

et al. 2016

ApJ

Self Cite

187

182

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We report on a set of long-term general-relativistic three-dimensional (3D) multi-group (energy-dependent) neutrino radiation-hydrodynamics simulations of core-collapse supernovae. We employ a full 3D two-moment scheme with the local M1 closure, three neutrino species, and 12 energy groups per species. With this, we follow the post-core-bounce evolution of the core of a nonrotating - M 27 progenitor in full unconstrained 3D and in octant symmetry for 380 ms. We find the development of an asymmetric runaway explosion in our unconstrained simulation. We test the resolution dependence of our results and, in agreement with previous work, find that low resolution artificially aids explosion and leads to an earlier runaway expansion of the shock. At low resolution, the octant and full 3D dynamics are qualitatively very similar, but at high resolution, only the full 3D simulation exhibits the onset of explosion.

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Black Hole Formation in Failing Core-Collapse Supernovae

Cited by 713 publications

References 94 publications

Systematic features of axisymmetric neutrino-driven core-collapse supernova models in multiple progenitors

Systematic features of axisymmetric neutrino-driven core-collapse supernova models in multiple progenitors

On the formation of galactic black hole low-mass X-ray binaries

General-Relativistic Three-Dimensional Multi-Group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae

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