Effects of Rotation on Standing Accretion Shock Instability in Nonlinear Phase for Core-Collapse Supernovae

Iwakami, Wakana; Kotake, Kei; Ohnishi, Naofumi; Yamada, Shoichi; Sawada, Keisuke

doi:10.1088/0004-637x/700/1/232

Cited by 78 publications

(57 citation statements)

References 40 publications

(64 reference statements)

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“…A fourth group has used a version of the Zeus-MP code (Hayes et al 2006;Iwakami et al 2008Iwakami et al , 2009a for hydrodynamics and the IDSA scheme for neutrino transport (Liebendörfer et al 2009), which we will refer to as "Zeus +IDSA." Zeus+IDSA is fully Newtonian and the transport omits inelastic (energy exchanging) scattering in favor of the elastic versions.…”

Section: Other Axisymmetric Simulationsmentioning

confidence: 99%

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Bruenn

Lentz

Hix

et al. 2016

ApJ

203

300

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We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25 M  zero-age main sequence progenitors. All of the simulations yield explosions and havebeen evolved for at least 1.2 s after core bounce and 1 s after material first becomes unbound. These simulations were computed with our CHIMERA code employing RbR spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 s after core bounce allows the explosions to develop more fully and the processes involved in powering the explosions to become more clearly evident. We compute explosion energy estimates, including the negative gravitational binding energy of the stellar envelope outside the expanding shock, of 0.34, 0.88, 0.38, and 0.70 Bethe (B≡10 51 erg) and increasing at 0.03, 0.15, 0.19, and 0.52 B s 1 -, respectively, for the 12, 15, 20, and 25 M  models at the endpoint of this report. We examine the growth of the explosion energy in our models through detailed analyses of the energy sources and flows. We discuss how the explosion energies may be subject to stochastic variations as exemplfied by the effect of the explosion geometry of the 20 M  model in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. We compare our results for the explosion energies and ejected Ni 56 masses against some observational standards despite the large error bars in both models and observations.

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Section: Other Axisymmetric Simulationsmentioning

confidence: 99%

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Bruenn

Lentz

Hix

et al. 2016

ApJ

203

300

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“…It is possible that faster NS rotation requires the progenitor core to rotate (e.g., Heger et al 2005;Ott et al 2006). In a rotating environment, however, the growth of SASI spiral modes will be severely altered and potentially fostered (Blondin & Mezzacappa 2007;Yamasaki & Foglizzo 2008;Iwakami et al 2009), and three-dimensional simulations are therefore indispensable to make predictions for the connection between progenitor and NS rotation. Fryer & Kusenko (2006) pointed out that ejecta asymmetries could be used to distinguish between different theoretical suggestions for the kick mechanism.…”

Section: Neutron Star Spin-up Mechanismmentioning

confidence: 99%

Three-dimensional neutrino-driven supernovae: Neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products

Wongwathanarat

Janka

Müller

2013

A&A

279

376

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We present three-dimensional (3D) simulations of supernova explosions of nonrotating stars, triggered by the delayed neutrinoheating mechanism with a suitable choice of the core-neutrino luminosity. Our results show that asymmetric mass ejection caused by hydrodynamic instabilities can accelerate the neutron star (NS) up to recoil velocities of more than 700 km s −1 by the "gravitational tug-boat mechanism", which is sufficient to explain most observed pulsar space velocities. The associated NS spin periods for our nonrotating progenitors are about 100 ms to 8000 ms without any obvious correlation between spin and kick magnitudes or directions. This suggests that faster spins and a possible spin-kick alignment might require angular momentum in the progenitor core prior to collapse. Our simulations for the first time demonstrate a clear correlation between the size of the NS kick and anisotropic production and distribution of heavy elements created by explosive burning behind the shock. In the case of large pulsar kicks, the explosion is significantly stronger opposite to the kick vector. Therefore the bulk of the explosively fused iron-group elements, in particular nickel, are ejected mostly in large clumps against the kick direction. This contrasts with the case of low recoil velocity, where the nickelrich lumps are more isotropically distributed. Explosively produced intermediate-mass nuclei heavier than 28 Si (like 40 Ca and 44 Ti) also exhibit significant enhancement in the hemisphere opposite to the direction of fast NS motion, while the distribution of 12 C, 16 O, and 20 Ne is not affected, and that of 24 Mg only marginally. Mapping the spatial distribution of the heavy elements in supernova remnants with identified pulsar motion may offer an important diagnostic test of the kick mechanism. Unlike kick scenarios based on anisotropic neutrino emission, our hydrodynamical acceleration model predicts enhanced ejection of iron-group elements and of their nuclear precursors in the opposite direction to the NS recoil.

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“…, }) are excited as well, leading to more complex dynamics and smaller saturation amplitudes for individual modes (Iwakami et al 2008). In some 3D simulations, in particular in those that include some initial rotation, a strong spiral mode ( = 1, m = ±1), capable of redistributing angular momentum, has been observed (Blondin & Mezzacappa 2007;Iwakami et al 2008Iwakami et al , 2009Fernández 2010;Wongwathanarat et al 2010;Rantsiou et al 2011).…”

Section: Introductionmentioning

confidence: 99%

General-Relativistic Simulations of Three-Dimensional Core-Collapse Supernovae

Ott

Abdikamalov

Mösta

et al. 2013

ApJ

194

241

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We study the three-dimensional (3D) hydrodynamics of the post-core-bounce phase of the collapse of a 27 M star and pay special attention to the development of the standing accretion shock instability (SASI) and neutrino-driven convection. To this end, we perform 3D general-relativistic simulations with a three-species neutrino leakage scheme. The leakage scheme captures the essential aspects of neutrino cooling, heating, and lepton number exchange as predicted by radiation-hydrodynamics simulations. The 27 M progenitor was studied in 2D by Müller et al., who observed strong growth of the SASI while neutrino-driven convection was suppressed. In our 3D simulations, neutrino-driven convection grows from numerical perturbations imposed by our Cartesian grid. It becomes the dominant instability and leads to large-scale non-oscillatory deformations of the shock front. These will result in strongly aspherical explosions without the need for large-scale SASI shock oscillations. Low--mode SASI oscillations are present in our models, but saturate at small amplitudes that decrease with increasing neutrino heating and vigor of convection. Our results, in agreement with simpler 3D Newtonian simulations, suggest that once neutrino-driven convection is started, it is likely to become the dominant instability in 3D. Whether it is the primary instability after bounce will ultimately depend on the physical seed perturbations present in the cores of massive stars. The gravitational wave signal, which we extract and analyze for the first time from 3D general-relativistic models, will serve as an observational probe of the postbounce dynamics and, in combination with neutrinos, may allow us to determine the primary hydrodynamic instability.

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Effects of Rotation on Standing Accretion Shock Instability in Nonlinear Phase for Core-Collapse Supernovae

Cited by 78 publications

References 40 publications

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Three-dimensional neutrino-driven supernovae: Neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products

General-Relativistic Simulations of Three-Dimensional Core-Collapse Supernovae

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