Standing accretion shock instability: numerical simulations of core-collapse supernova

Ohnishi, Naofumi; Iwakami, Wakana; Kotake, Kei; Yamada, Shoichi; Fujioka, Shinsuke; Takabe, H.

doi:10.1088/1742-6596/112/4/042018

Cited by 8 publications

(9 citation statements)

References 13 publications

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“…17 Such study is obviously necessary for the analysis of the laboratory-astrophysics experiments proposed in Ref. 16. …”

Section: Discussionmentioning

confidence: 99%

“…Under the ICF/HEDP experimental conditions the mechanism of plasma stagnation via the expanding accretion shock is the same, although the gravity does not play a role in its acceleration. Still, there is a sufficient similarity to justify the recently proposed laboratory-astrophysics experiments 16 aimed at observing the so-called standing accretion shock instability 17 in a laser-driven plasma stagnating via a hemispherical shock wave.…”

Section: Introductionmentioning

confidence: 99%

“…37, where such analysis has been done for a converging shock wave. Stability analysis of other hydrodynamic 31 and MHD 32,33 generalizations of the classic Noh solution could shed light on the stability of hot-spot formation and other cases of shock-wave stagnation in laser-fusion and Z-pinch implosions, in laboratory astrophysics experiments, 16 as well as guide verification of hydrodynamic and MHD codes.…”

Section: Introductionmentioning

confidence: 99%

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Stability of stagnation via an expanding accretion shock wave

et al. 2016

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Stagnation of a cold plasma streaming to the center or axis of symmetry via an expanding accretion shock wave is ubiquitous in inertial confinement fusion (ICF) and high-energy- (2014)]. Some experimental evidence indicates that stagnation via an expanding shock wave is stable, but its stability has never been studied theoretically. We present such analysis for the stagnation that does not involve a rarefaction wave behind the expanding shock front and is described by the classic ideal-gas Noh solution in spherical and cylindrical geometry. In either case the stagnated flow has been demonstrated to be stable, initial perturbations exhibiting a powerlaw, oscillatory or monotonic, decay with time for all the eigenmodes. This conclusion has been supported by our simulations done both on a Cartesian grid and on a curvilinear grid in spherical coordinates. Dispersion equation determining the eigenvalues of the problem and explicit formulas for the eigenfunction profiles corresponding to these eigenvalues are presented, making it possible to use the theory for hydro code verification in two and three dimensions.

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“…17 Such study is obviously necessary for the analysis of the laboratory-astrophysics experiments proposed in Ref. 16. …”

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Stability of stagnation via an expanding accretion shock wave

et al. 2016

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“…These perturbations are converted to sound waves at the PNS surface which propagate back up to the shock and give rise to new perturbations. Under the right conditions this cycle grows in amplitude and results in large-scale quasi-periodic oscillations of the shock (Blondin et al 2003;Blondin & Mezzacappa 2006;Foglizzo et al 2007;Ohnishi et al 2006Ohnishi et al , 2008Scheck et al 2008;Guilet & Foglizzo 2012;Foglizzo et al 2015). The typical time scale, τ, of the SASI is given by the time it takes a perturbation to be advected from the shock-front plus the time needed for the sound waves to propagate back upstream to the shock.…”

Section: The Characteristics Of Gravitational Waves Frommentioning

confidence: 99%

Gravitational-wave signals from 3D supernova simulations with different neutrino-transport methods

Andresen

Glas

Janka

2021

Monthly Notices of the Royal Astronomical Society

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We compare gravitational-wave (GW) signals from eight three-dimensional simulations of core-collapse supernovae, using two different progenitors with zero-age main sequence masses of 9 and 20 solar masses (M⊙). The collapse of each progenitor was simulated four times, at two different grid resolutions and with two different neutrino transport methods, using the Aenus-Alcar code. The main goal of this study is to assess the validity of recent concerns that the so-called “Ray-by-Ray+” (RbR+) approximation is problematic in core-collapse simulations and can adversely affect theoretical GW predictions. Therefore, signals from simulations using RbR+ are compared to signals from corresponding simulations using a fully multidimensional (FMD) transport scheme. The 9M⊙ progenitor successfully explodes, whereas the 20M⊙ model does not. Both the standing accretion shock instability and hot-bubble convection develop in the postshock layer of the non-exploding models. In the exploding models, neutrino-driven convection in the postshock flow is established around 100 ms after core bounce and lasts until the onset of shock revival. We can, therefore, judge the impact of the numerical resolution and neutrino transport under all conditions typically seen in non-rotating core-collapse simulations. We find excellent qualitative agreement in all GW features. We find minor quantitative differences between simulations, but find no systematic differences between simulations using different transport schemes. Resolution-dependent differences in the hydrodynamic behaviour of low-resolution and high-resolution models have a greater impact on the GW signals than consequences of the different transport methods. Furthermore, increasing the resolution decreases the discrepancies between models with different neutrino transport.

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“…One particular experimental realization of the standing accretion shock (SAS) model has been proposed recently by Ohnishi et al [31]. In Ohnishi's design, supersonic converging flow is created by deposition of laser energy at the outer surface of the target.…”

Section: Proposed Experimental Designmentioning

confidence: 99%