Is Strong Sasi Activity the Key to Successful Neutrino-Driven Supernova Explosions?

Hanke, Florian; Marek, Andreas; Müller, Bernhard; Janka, Hans-Thomas

doi:10.1088/0004-637x/755/2/138

Cited by 207 publications

(480 citation statements)

References 53 publications

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Mentioning

411

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“…It should be noted that the mass accretion rate of the WW15 model shows a sudden drop from 0.8 M ⊙ s −1 to 0.3 M ⊙ s −1 at t pb ∼ 150 ms (t pb ; postbounce time) then gradually decreases to 0.2 M ⊙ s −1 . This is in a good agreement with the previous results using the same progenitor model (e.g., Figure 1 in Murphy & Burrows (2008) and Figure 1 in Hanke et al (2012)). All of these facts support that our boundary conditions well imitate the density structure out of the boundary of these three 15 M ⊙ models and the boundary effect is not significant for these models.…”

Section: Boundary Conditionsupporting

confidence: 93%

“…After that, the accretion rate gradually decreases to ∼ 0.1 M ⊙ s −1 till t 400 = 420 ms at this time the revived shock has expanded to an average ra-dius of r = 400 km. Here t 400 is a useful measure to qualify the vigor of the shock revival (e.g., Hanke et al 2012). On the other hand, model s21.0 has high compactness (ξ 2.0 = 0.46), which leads to the high accretion rate (black dashed line in Figure 8).…”

Section: Resultsmentioning

confidence: 99%

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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

128

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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: Boundary Conditionsupporting

confidence: 93%

Section: Resultsmentioning

confidence: 99%

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

128

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show abstract

“…convection and the SASI lead to a reduction of the critical luminosity (see, e.g. Janka & Müller 1996;Herant et al 1992;Nordhaus et al 2010;Hanke et al 2012;Couch 2013).…”

Section: Explosion In Dependence Of the Magnetic Fieldmentioning

confidence: 99%

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Obergaulinger¹,

Janka²,

Aloy³

2014

Monthly Notices of the Royal Astronomical Society

105

117

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We study the amplification of magnetic fields in the collapse and the post-bounce evolution of the core of a non-rotating star of 15 M in axisymmetry. To this end, we solve the coupled equations of magnetohydrodynamics and neutrino transport in the two-moment approximation. The pre-collapse magnetic field is strongly amplified by compression in the infall. Initial fields of the order of 10 10 G translate into proto-neutron star fields similar to the ones observed in pulsars, while stronger initial fields yield magnetar-like final field strengths. After core bounce, the field is advected through the hydrodynamically unstable neutrino-heating layer, where non-radial flows due to convection and the standing accretion shock instability amplify the field further. Consequently, the resulting amplification factor of order five is the result of the number of small-eddy turnovers taking place within the time scale of advection through the post-shock layer. Due to this limit, most of our models do not reach equipartition between kinetic and magnetic energy and, consequently, evolve similarly to the non-magnetic case, exploding after about 800 ms when a single or few highentropy bubbles persist over several dynamical time scales. In the model with the strongest initial field we studied, 10 12 G, for which equipartition between flow and field is achieved, the magnetic tension favours a much earlier development of such long-lived high-entropy bubbles and enforces a fairly ordered large-scale flow pattern. Consequently, this model, after exhibiting very regular shock oscillations, explodes much earlier than non-magnetic ones.

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“…Imposing symmetries on simulations of CCSNe can have significant consequences for their evolution (e.g., Hanke et al 2012;Couch 2013;Murphy et al 2013). Detailed spherically symmetric one-dimensional (1D) simulations do not explode (Liebendörfer et al 2001), except when particular low-mass progenitor models are used (e.g., Fischer et al 2010;Hüdepohl et al 2010).…”

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

188

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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Is Strong Sasi Activity the Key to Successful Neutrino-Driven Supernova Explosions?

Cited by 207 publications

References 53 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

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

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

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