CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK-HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE

AbstractAfter the Big Bang, production of heavy elements in the early Universe takes place in the first stars and their supernova explosions. The nature of the first supernovae, however, has not been well understood. The signature of nucleosynthesis yields of the first supernovae can be seen in the elemental abundance patterns observed in extremely metal-poor stars. Interestingly, those abundance patterns show some peculiarities relative to the solar abundance pattern, which should provide important clues to understanding the nature of early generations of supernovae. We review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars.

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Applying the jet feedback mechanism to core-collapse supernova explosions

Monthly Notices of the Royal Astronomical Society ◽

10.1111/j.1365-2966.2009.15862.x ◽

2010 ◽

Vol 401 (4) ◽

pp. 2793-2798 ◽

Cited By ~ 15

Author(s):

Noam Soker

Keyword(s):

Feedback Mechanism ◽

Core Collapse ◽

Core Collapse Supernova ◽

Supernova Explosions

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Global Anisotropy versus Small‐Scale Fluctuations in Neutrino Flux in Core‐Collapse Supernova Explosions

The Astrophysical Journal ◽

10.1086/375833 ◽

2003 ◽

Vol 592 (2) ◽

pp. 1035-1041 ◽

Cited By ~ 5

Author(s):

Hideki Madokoro ◽

Tetsuya Shimizu ◽

Yuko Motizuki

Keyword(s):

Neutrino Flux ◽

Small Scale ◽

Core Collapse ◽

Core Collapse Supernova ◽

Supernova Explosions

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The SuperN-Project: Porting and Optimizing VERTEX-PROMETHEUS on the Cray XE6 at HLRS for Three-Dimensional Simulations of Core-Collapse Supernova Explosions of Massive Stars

High Performance Computing in Science and Engineering ‘12 ◽

10.1007/978-3-642-33374-3_8 ◽

2012 ◽

pp. 81-93

Author(s):

F. Hanke ◽

A. Marek ◽

B. Müller ◽

H.-Th. Janka

Keyword(s):

Massive Stars ◽

Three Dimensional ◽

Core Collapse ◽

Core Collapse Supernova ◽

Supernova Explosions ◽

Three Dimensional Simulations

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Effects of Small-Scale Fluctuations of Neutrino Flux in Supernova Explosions

International Astronomical Union Colloquium ◽

10.1017/s0252921100009349 ◽

2005 ◽

Vol 192 ◽

pp. 309-314

Author(s):

Hideki Madokoro ◽

Tetsuya Shimizu ◽

Yuko Motizuki

Keyword(s):

Neutrino Flux ◽

Explosion Energy ◽

Small Scale ◽

Core Collapse ◽

Effective Mechanism ◽

Core Collapse Supernova ◽

Neutrino Radiation ◽

Spherical Explosion ◽

Supernova Explosions ◽

Neutrino Luminosity

SummaryWe examine effects of small-scale fluctuations with angle in the neutrino radiation in core-collapse supernova explosions. As the mode number of fluctuations increases, the results approach those of spherical explosion. We conclude that global anisotropy of the neutrino radiation is the most effective mechanism of increasing the explosion energy when the total neutrino luminosity is given.

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Acoustic wave generation in collapsing massive stars with convective shells

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa533 ◽

2020 ◽

Vol 493 (3) ◽

pp. 3496-3512 ◽

Cited By ~ 1

Author(s):

Ernazar Abdikamalov ◽

Thierry Foglizzo

Keyword(s):

Acoustic Waves ◽

Massive Stars ◽

Core Collapse ◽

Core Collapse Supernova ◽

Stellar Collapse ◽

Acoustic Wave Generation ◽

Supernova Explosions ◽

Accretion Shock ◽

Stationary Background ◽

Hydrodynamics Equations

ABSTRACT The convection that takes place in the innermost shells of massive stars plays an important role in the formation of core-collapse supernova explosions. Upon encountering the supernova shock, additional turbulence is generated, amplifying the explosion. In this work, we study how the convective perturbations evolve during the stellar collapse. Our main aim is to establish their physical properties right before they reach the supernova shock. To this end, we solve the linearized hydrodynamics equations perturbed on a stationary background flow. The latter is approximated by the spherical transonic Bondi accretion, while the convective perturbations are modelled as a combination of entropy and vorticity waves. We follow their evolution from large radii, where convective shells are initially located, down to small radii, where they are expected to encounter the accretion shock above the proto-neutron star. Considering typical vorticity perturbations with a Mach number ∼0.1 and entropy perturbations with magnitude ∼0.05kb/baryon, we find that the advection of these perturbations down to the shock generates acoustic waves with a relative amplitude $\delta {\rm p}/\gamma {\rm p} \lesssim 10{{\ \rm per\ cent}}$, in agreement with published numerical simulations. The velocity perturbations consist of contributions from acoustic and vorticity waves with values reaching ${\sim}10{{\ \rm per\ cent}}$ of the sound speed ahead of the shock. The perturbation amplitudes decrease with increasing ℓ and initial radii of the convective shells.

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The Status of Multi-Dimensional Core-Collapse Supernova Models

Publications of the Astronomical Society of Australia ◽

10.1017/pasa.2016.40 ◽

2016 ◽

Vol 33 ◽

Cited By ~ 121

Author(s):

B. Müller

Keyword(s):

Initial Conditions ◽

Massive Stars ◽

Core Collapse ◽

Solar Mass ◽

Convective Boundary ◽

3D Simulations ◽

Core Collapse Supernova ◽

Wide Range ◽

Supernova Explosions ◽

The Impact

AbstractModels of neutrino-driven core-collapse supernova explosions have matured considerably in recent years. Explosions of low-mass progenitors can routinely be simulated in 1D, 2D, and 3D. Nucleosynthesis calculations indicate that these supernovae could be contributors of some lighter neutron-rich elements beyond iron. The explosion mechanism of more massive stars remains under investigation, although first 3D models of neutrino-driven explosions employing multi-group neutrino transport have become available. Together with earlier 2D models and more simplified 3D simulations, these have elucidated the interplay between neutrino heating and hydrodynamic instabilities in the post-shock region that is essential for shock revival. However, some physical ingredients may still need to be added/improved before simulations can robustly explain supernova explosions over a wide range of progenitors. Solutions recently suggested in the literature include uncertainties in the neutrino rates, rotation, and seed perturbations from convective shell burning. We review the implications of 3D simulations of shell burning in supernova progenitors for the ‘perturbations-aided neutrino-driven mechanism,’ whose efficacy is illustrated by the first successful multi-group neutrino hydrodynamics simulation of an 18 solar mass progenitor with 3D initial conditions. We conclude with speculations about the impact of 3D effects on the structure of massive stars through convective boundary mixing.

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