Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

Burrows, Adam; Vartanyan, David; Dolence, Joshua C.; Skinner, M. Aaron; Radice, David

doi:10.1007/s11214-017-0450-9

Cited by 140 publications

(171 citation statements)

References 127 publications

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“…yet converged (Ugliano et al 2012;Suwa et al 2016;Ertl et al 2016;Burrows et al 2018). This parameter is also important to predict the neutrino emission (Horiuchi et al 2017).…”

Section: Appendixmentioning

confidence: 72%

One-, Two-, and Three-dimensional Simulations of Oxygen-shell Burning Just before the Core Collapse of Massive Stars

Yoshida

Takiwaki

Kotake

et al. 2019

ApJ

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We perform two-(2D) and three-dimensional (3D) hydrodynamics simulations of convective oxygen shell-burning that takes place deep inside a massive progenitor star of a core-collapse supernova. Using one dimensional (1D) stellar evolution code, we first calculate the evolution of massive stars with an initial mass of 9-40 M . Four different overshoot parameters are applied, and CO core mass trend similar to previous works is obtained in the 1D models. Selecting eleven 1D models that have a silicon and oxygen coexisting layer, we perform 2D hydrodynamics simulations of the evolution for ∼100 s until the onset of core-collapse. We find that convection with large-scale eddies and the turbulent Mach number ∼0.1 is obtained in the models having a Si/O layer with a scale of 10 8 cm, whereas most models that have an extended O/Si layer up to a few ×10 9 cm exhibit lower turbulent velocity.Our results indicate that the supernova progenitors that possess a thick Si/O layer could provide a preferable condition for perturbation-aided explosions. We perform 3D simulation of a 25 M model, which exhibits large-scale convection in the 2D models. The 3D model develops large-scale ( = 2) convection similar to the 2D model, however, the turbulent velocity is lower. By estimating the neutrino emission properties of the 3D model, we point out that a time modulation of the event rates, if observed in KamLAND and Hyper-Kamiokande, would provide an important information about structural changes in the presupernova convective layer.

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“…yet converged (Ugliano et al 2012;Suwa et al 2016;Ertl et al 2016;Burrows et al 2018). This parameter is also important to predict the neutrino emission (Horiuchi et al 2017).…”

Section: Appendixmentioning

confidence: 72%

One-, Two-, and Three-dimensional Simulations of Oxygen-shell Burning Just before the Core Collapse of Massive Stars

Yoshida

Takiwaki

Kotake

et al. 2019

ApJ

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“…The numerical and physical details incorporated into the code Fornax have been published in numerous papers in recent years (Skinner et al 2016;Burrows et al 2018;Vartanyan et al 2018;Burrows et al 2019;Skinner et al 2019).…”

Section: Numerical Methods and Computational Setupmentioning

confidence: 99%

The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations

Burrows

Radice

Vartanyan

et al. 2019

Monthly Notices of the Royal Astronomical Society

268

230

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We have conducted nineteen state-of-the-art 3D core-collapse supernova simulations spanning a broad range of progenitor masses. This is the largest collection of sophisticated 3D supernova simulations ever performed. We have found that while the majority of these models explode, not all do, and that even models in the middle of the available progenitor mass range may be less explodable. This does not mean that those models for which we did not witness explosion would not explode in Nature, but that they are less prone to explosion than others. One consequence is that the "compactness" measure is not a metric for explodability. We find that lower-mass massive star progenitors likely experience lower-energy explosions, while the higher-mass massive stars likely experience higher-energy explosions. Moreover, most 3D explosions have a dominant dipole morphology, have a pinched, wasp-waist structure, and experience simultaneous accretion and explosion. We reproduce the general range of residual neutron-star masses inferred for the galactic neutron-star population. The most massive progenitor models, however, in particular visà vis explosion energy, need to be continued for longer physical times to asymptote to their final states. We find that while the majority of the inner ejecta have Y e = 0.5, there is a substantial proton-rich tail. This result has important implications for the nucleosynthetic yields as a function of progenitor. Finally, we find that the non-exploding models eventually evolve into compact inner configurations that experience a quasi-periodic spiral SASI mode. We otherwise see little evidence of the SASI in the exploding models.

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“…Pauli exclusion is included via the stimulated emission term in (Burrows et al 2006). We include the many-body correction (see also Burrows et al 2018) to neutrino-nucleon scattering following Horowitz et al (2017), which fits to high densities following Burrows & Sawyer (1998). For electron-positron pair annihilation and bremsstrahlung, which dominate heavy neutrino production, we follow Thompson et al (2000).…”

Section: Numerical Setupmentioning

confidence: 99%

Temporal and angular variations of 3D core-collapse supernova emissions and their physical correlations

Vartanyan

Burrows

Radice

2019

Monthly Notices of the Royal Astronomical Society

118

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We provide the time series and angular distributions of the neutrino and gravitationalwave emissions of eleven state-of-the-art three-dimensional non-rotating core-collapse supernova models and explore correlations between these signatures and the real-time dynamics of the shock and the proto-neutron-star core. The neutrino emissions are roughly isotropic on average, with instantaneous excursions about the mean inferred luminosity of as much as ±20%. The deviation from isotropy is least for the "ν µ "-type neutrinos and the lowest-mass progenitors. Instantaneous temporal luminosity variations along a given direction for exploding models average ∼2−4%, but can be as high as ∼10%. For non-exploding models, they can achieve ∼25%. The temporal variations in the neutrino emissions correlate with the temporal and angular variations in the mass accretion rate. We witness the LESA phenomenon in all our models and find that the vector direction of the LESA dipole and that of the inner Y e distribution are highly correlated. For our entire set of 3D models, we find strong connections between the cumulative neutrino energy losses, the radius of the proto-neutron star, and the f -mode frequency of the gravitational wave emissions. When physically normalized, the progenitor-to-progenitor variation in any of these quantities is no more than ∼10%. Moreover, the reduced f -mode frequency is independent of time after bounce to better than ∼10%. Therefore, simultaneous measurement of gravitational waves and neutrinos from a given supernova event can be used synergistically to extract real physical quantities of the supernova core.

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Crucial Physical Dependencies of the Core-Collapse Supernova Mechanism

Cited by 140 publications

References 127 publications

One-, Two-, and Three-dimensional Simulations of Oxygen-shell Burning Just before the Core Collapse of Massive Stars

One-, Two-, and Three-dimensional Simulations of Oxygen-shell Burning Just before the Core Collapse of Massive Stars

The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations

Temporal and angular variations of 3D core-collapse supernova emissions and their physical correlations

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