A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE

By T. Takiwaki, K. Kotake, Y. Suwa. 2013

171 citations recorded by the source corpus.

We present numerical results on two- (2D) and three-dimensional (3D) hydrodynamic core-collapse simulations of an 11.2 M☉ star. By changing numerical resolutions and seed perturbations systematically, we study how the postbounce dynamics are different in 2D and 3D. The calculations were performed with an energy-dependent treatment of the neutrino transport based on the isotropic diffusion source approximation scheme, which we have updated to achieve a very high computational efficiency. All of the computed models in this work, including nine 3D models and fifteen 2D models, exhibit the revival of the stalled bounce shock, leading to the possibility of explosion. All of them are driven by the neutrino-heating mechanism, which is fostered by neutrino-driven convection and the standing-accretion-shock instability. Reflecting the stochastic nature of multi-dimensional (multi-D) neutrino-driven explosions, the blast morphology changes from model to model. However, we find that the final fate of the multi-D models, whether an explosion is obtained or not, is little affected by the explosion stochasticity. In agreement with some previous studies, higher numerical resolutions lead to slower onset of the shock revival in both 2D and 3D. Based on the self-consistent supernova models leading to the possibility of explosions, our results systematically show that the revived shock expands more energetically in 2D than in 3D.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/439be1019cc95e2995f9338487e578fe238311aa

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Citations in the corpus

THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “Early versions neglectedνµτ and ν̄µτ completely, but some recent works (Takiwaki et al. 2014; Nakamura et al. 2014b) have included a leakage scheme for these species.”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, methodology): “…explosion, these oscillations, tentatively identiﬁed as l = 2 surface g modes by M¨uller et al. (2013), are primarily driven by the downﬂows imping-1 Takiwaki et al. (2012, 2014) employ the isotropic diffusion source approximation (Liebend¨orfer, Whitehouse & Fischer 2009) and use further…”
Global comparison of core-collapse supernova simulations in spherical symmetry (2018, methodology): “[30] Tomoya Takiwaki, Kei Kotake, and Yudai Suwa.”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “…CCSNe with stateof-the-art neutrino physics have been recently performed by a number of groups (Melson et al. 2015b,a; Lentz et al. 2015; Müller et al. 2017; Ott et al. 2017; see also Takiwaki et al. 2012; Ott et al. 2013; Takiwaki et al. 2014; Müller 2015; Roberts et al. 2016; Pan et al. 2017).”
THE ROLE OF TURBULENCE IN NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2014, background): “…mechanism (e.g., Burrows et al. 1995; Murphy & Burrows 2008; Marek & Janka 2009; Dolence et al. 2013; Müller et al. 2012b; Bruenn et al. 2013; Takiwaki et al. 2014): multi-dimensional motions increase the dwell time of material in the gain region, enhance the efficiency of neutrino heating,…”
NEUTRINO-DRIVEN EXPLOSION OF A 20 SOLAR-MASS STAR IN THREE DIMENSIONS ENABLED BY STRANGE-QUARK CONTRIBUTIONS TO NEUTRINO–NUCLEON SCATTERING (2015, background): “…(e.g., Hanke et al. 2012; Couch 2013; Couch & O’Connor 2014; Couch & Ott 2015) and self-consistent simulations with approximate neutrino transport (Takiwaki et al. 2012, 2014), which revealed that the onset of explosion is less favored or delayed in 3D compared to 2D, contradicting claims by…”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “…now been observed in a sizable number of 3D simulations by different groups employing multi-group transport with varying degrees of sophistication (Takiwaki et al. 2012, 2014; Melson et al. 2015a,b; Müller 2015; Lentz et al. 2015; Roberts et al. 2016; Müller et al. 2017a; Ott et al. 2018; Chan…”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “However, because of the turbulent nature of CCSNe and on the basis of previous studies that have employed simplified microphysics (Hanke et al. 2012; Takiwaki et al. 2014; Abdikamalov et al. 2015; Radice et al. 2016), we expect that the detailed quantitative evolution of each model will be…”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, result): “…to 2D calculations or even no explosions (e.g., Hanke et al. 2012, 2013; Tamborra et al. 2014; Mezzacappa et al. 2015; Couch 2013; Couch & O’Connor 2014; Takiwaki et al. 2014) although some studies have proclaimed the opposite behavior (Nordhaus et al. 2010; Burrows 2013; Dolence et al. 2013).”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, methodology): “Some simulations disregard heavy flavour neutrinos altogether (e.g Suwa et al. 2010; Takiwaki et al. 2012), or only treat them by means of a leakage scheme (Takiwaki et al. 2014; Pan et al. 2016).”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, methodology): “…various algorithms for multi-group neutrino transport ranging from the very rigorous Vertex (Hanke et al. 2013; Melson et al. 2015a,b; Janka et al. 2016) and Chimera (Lentz et al. 2015) models to more approximate methods (Takiwaki et al. 2012, 2014, 2016; Müller 2015; Roberts et al. 2016).”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, background): “…a neutrino-light bulb description with simple heating and cooling terms (Hanke et al. 2012; Couch 2013), rayby-ray neutrino trapping with a parameterized heating strength (Couch & O’Connor 2014), and a ray-by-ray implementation of the isotropic diffusion source approximation (Takiwaki et al. 2014).”
THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVA SIMULATED USING A 15 M⊙ PROGENITOR (2015, methodology): “A 2.7◦ angular resolution follow-up using the same progenitor (Takiwaki et al. 2014) also initiated explosions that subsequently developed more slowly than corresponding 2D simulations.”
NEUTRINO-DRIVEN SUPERNOVA OF A LOW-MASS IRON-CORE PROGENITOR BOOSTED BY THREE-DIMENSIONAL TURBULENT CONVECTION (2015, background): “…influence of 3D turbulence observed in previous studies of more massive stars (e.g., Hanke et al. 2012; Couch 2013; Couch & O’Connor 2014; Takiwaki et al. 2012, 2014; Abdikamalov et al. 2014), the decrease of the mass inflow rate through the gain radius and reduced neutrino-energy loss…”