SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES

By Florian Hanke, Bernhard Müller, A. Wongwathanarat, Andreas Marek, Hans-Thomas Janka. 2013

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The relevance of the standing accretion shock instability (SASI) compared to neutrino-driven convection in three-dimensional (3D) supernova-core environments is still highly controversial. Studying a 27 M☉ progenitor, we demonstrate, for the first time, that violent SASI activity can develop in 3D simulations with detailed neutrino transport despite the presence of convection. This result was obtained with the Prometheus-Vertex code with the same sophisticated neutrino treatment so far used only in one-dimensional and two-dimensional (2D) models. While buoyant plumes initially determine the nonradial mass motions in the postshock layer, bipolar shock sloshing with growing amplitude sets in during a phase of shock retraction and turns into a violent spiral mode whose growth is only quenched when the infall of the Si/SiO interface leads to strong shock expansion in response to a dramatic decrease of the mass accretion rate. In the phase of large-amplitude SASI sloshing and spiral motions, the postshock layer exhibits nonradial deformation dominated by the lowest-order spherical harmonics (ℓ = 1, m = 0, ±1) in distinct contrast to the higher multipole structures associated with neutrino-driven convection. We find that the SASI amplitudes, shock asymmetry, and nonradial kinetic energy in three dimensions can exceed those of the corresponding 2D case during extended periods of the evolution. We also perform parameterized 3D simulations of a 25 M☉ progenitor, using a simplified, gray neutrino transport scheme, an axis-free Yin-Yang grid, and different amplitudes of random seed perturbations. They confirm the importance of the SASI for another progenitor, its independence of the choice of spherical grid, and its preferred growth for fast accretion flows connected to small shock radii and compact proto-neutron stars as previously found in 2D setups.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/923028ab6a34b17988d2916e3d52be3703c9fb95

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Citations in the corpus

THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVA SIMULATED USING A 15 M⊙ PROGENITOR (2015, methodology): “M progenitors (Hanke et al. 2013) produce explosions where their 3D counterparts do not.”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, methodology): “(i) s27-2D:models27-2Dwassimulatedwiththesamenumerical setup as s27 (see Hanke et al. 2013), with an initial grid resolution of 400 × 88 zones in r and θ and the innermost 10km being simulated in spherical symmetry to allow for optimal comparison with the 3D model.”
A simple approach to the supernova progenitor–explosion connection (2016, background): “…successes in 3D explosion modelling (Melson, Janka & Marek 2015a ; Melson et al. 2015b; Lentz et al. 2015 ; M¨uller 2015), obtaining explosions has proved more difﬁcult in 3D multigroup neutrino transport models than in 2D (Hanke et al. 2013; Tamborra et al. 2014; Takiwaki, Kotake & Suwa 2014).”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, methodology): “This feature is qualitatively consistent with the 2D self-consistent models by Marek & Janka (2009) and with the 3D idealized models by Hanke et al. (2013); Couch (2013), respectively. σ400 in Table 1 represents the model dispersion of t400, which varies much more stochastically in 3D models with…”
NEUTRINO-DRIVEN SUPERNOVA OF A LOW-MASS IRON-CORE PROGENITOR BOOSTED BY THREE-DIMENSIONAL TURBULENT CONVECTION (2015, background): “S R ] 1 9 Fe b 20 15 plied in 3D also by Hanke et al. (2013) and Tamborra et al. (2014), in particular the high-density equation of state of Lattimer & Swesty (1991) with a nuclear incompressibility of K = 220 MeV.”
Science case for the Einstein telescope (2019, background): “The three-flavor neutrino flux emanating from the proto-neutron star could power itself a core collapse supernova via neutrino heating on delayed timescales of order one second [104–116].”
REVIVAL OF THE STALLED CORE-COLLAPSE SUPERNOVA SHOCK TRIGGERED BY PRECOLLAPSE ASPHERICITY IN THE PROGENITOR STAR (2013, background): “…that convection and the standing accretion shock instability (SASI) robustly break spherical symmetry in the pre-explosion stalled-shock phase (see, e.g., Couch & O’Connor 2013; Couch 2013; Ott et al. 2013; Dolence et al. 2013; Hanke et al. 2013; Takiwaki et al. 2013 for recent 3D simulations).”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “…with spectral, ray-by-ray neutrino transport, approximate general relativity, and state-of-the-art weak interactions are underway, and the results from early stages of the post-bounce dynamics have been reported by Hanke et al. (2013), using VERTEX, and Mezzacappa et al. (2014), using CHIMERA.”
NEUTRINO-DRIVEN EXPLOSION OF A 20 SOLAR-MASS STAR IN THREE DIMENSIONS ENABLED BY STRANGE-QUARK CONTRIBUTIONS TO NEUTRINO–NUCLEON SCATTERING (2015, background): “However, previous 3D simulations of this group for 11.2, 20, and 27 M progenitors had not produced explosions until ∼400–550 ms after bounce, although corresponding 2D models had exploded (Hanke et al. 2013; Tamborra et al. 2013, 2014a,b).”
What can be learned from a future supernova neutrino detection (2017, background): “the SASI can also develop a spiral mode which is seen to aid the explosion [133, 134].”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, methodology): “…3D core-collapse supernova simulations employing 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.…”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, background): “…is even more diffuse because current 3D simulations agree in showing slower explo- sions compared 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…”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “…convection (Burrows et al. 1995; Janka & Mueller 1996; Foglizzo et al. 2006; Radice et al. 2016, 2018), or the standing accretion shock instability (SASI; Blondin et al. 2003; Foglizzo et al. 2007; Burrows et al. 2012; Hanke et al. 2013; Abdikamalov et al. 2015) become fully developed.”
THE ROLE OF TURBULENCE IN NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2014, background): “The handful of 3D simulations including sophisticated neutrino transport have somewhat dashed those hopes, however, as they fail to explode, even for progenitors that explode in 2D (Hanke et al. 2013; Tamborra et al. 2014).”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, methodology): “…not possess the violent SASI episodes that massively affect the neutrino-emission properties in the 20 and 27 M cases (Tamborra et al. 2013, 2014; Hanke et al. 2013), where they lead to time-dependent variations of the neutrino transport and radiation, superimposed on the hemispheric asymmetry…”
Long-Baseline Neutrino Facility (LBNF) and Deep Underground Neutrino Experiment (DUNE) Conceptual Design Report Volume 1: The LBNF and DUNE Projects (2015, background): “• The standing accretion shock instability (SASI) [156, 157], a “sloshing” mode predicted by three-dimensional neutrino-hydrodynamics simulations of supernova cores, would give an oscillatory flavor-dependent modulation of the flux.”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “…to compute artificially initiated neutrino-driven explosions was not favorable for strong SASI activity, although in self-consistent simulations phases of SASI sloshing and spiral motions are found to be prevalent for many models (e.g. Hanke et al. 2013; Tamborra et al. 2014b; Kuroda et al. 2016).”
Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume II: DUNE Physics (2020, background): “• The standing accretion shock instability (SASI) [265, 266], a “sloshing” mode predicted by three-dimensional neutrino-hydrodynamics simulations of supernova cores, would give an oscillatory flavor-dependent modulation of the flux.”
Long-Baseline Neutrino Facility (LBNF) and Deep Underground Neutrino Experiment (DUNE) Conceptual Design Report Volume 2: The Physics Program for DUNE at LBNF (2015, background): “• The standing accretion shock instability (SASI) [156, 157], a “sloshing” mode predicted by three-dimensional neutrino-hydrodynamics simulations of supernova cores, would give an oscillatory flavor-dependent modulation of the flux.”