THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT

By T. Takiwaki, K. Kotake, Y. Suwa. 2011

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We present numerical results on three-dimensional (3D) hydrodynamic core-collapse simulations of an 11.2 M☉ star. By comparing one-dimensional (1D) and two-dimensional (2D) results with those of 3D, we study how the increasing spacial multi-dimensionality affects the postbounce supernova dynamics. The calculations were performed with an energy-dependent treatment of the neutrino transport that is solved by the isotropic diffusion source approximation scheme. In agreement with previous study, our 1D model does not produce explosions for the 11.2 M☉ star, while the neutrino-driven revival of the stalled bounce shock is obtained in both the 2D and 3D models. The standing accretion-shock instability (SASI) is observed in the 3D models, in which the dominant mode of the SASI is bipolar (ℓ = 2) with its saturation amplitudes being slightly smaller than 2D. By performing a tracer-particle analysis, we show that the maximum residency time of material in the gain region becomes longer in 3D than in 2D due to non-axisymmetric flow motions, which is one of advantageous aspects of 3D models to obtain neutrino-driven explosions. Our results show that convective matter motions below the gain radius become much more violent in 3D than in 2D, making the neutrino luminosity larger for 3D. Nevertheless, the emitted neutrino energies are made smaller due to the enhanced cooling. Our results indicate whether these advantages for driving 3D explosions could or could not overwhelm the disadvantages is sensitive to the employed numerical resolutions. An encouraging finding is that the shock expansion tends to become more energetic for models with finer resolutions. To draw a robust conclusion, 3D simulations with much higher numerical resolutions and with more advanced treatment of neutrino transport and of gravity are needed, which could be practicable by utilizing forthcoming Petaflops-class supercomputers.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8c2a4e1d12c3713fada136564dc054be23872580

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Citations in the corpus

A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, background): “…redshift, ray-by-ray transport vs. multi-angle transport), the neutrino processes (e.g. omission of µ/τ neutrinos in Suwa et al. 2010 and Takiwaki et al. 2012), the hydro solver (high-resolution shock capturing schemes vs. artificial viscosity), or the treatment of gravity (effective…”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “…approach that better quantifies the complexities of the multidimensional flows is to examine the evolution of the residency time distribution function of the included passive tracer particles (Murphy & Burrows 2008; Takiwaki et al. 2012; Handy et al. 2014), which we will examine in a later paper.”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, methodology): “Recent Newtonian simulations by Takiwaki et al. (2012) and GR simulations by Kuroda et al. (2012) and Ott et al. (2012) are first, tentative steps to higher sophistication in 3D models, but these works were still focused on a few progenitors only and employed crude neutrino transport methods with…”
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…”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, methodology): “If convection does develop, a simple measure of its strength is the anisotropic velocity vaniso, which we define, following Takiwaki et al. (2012), as vaniso = √√√√ 〈 ρ [( vr − 〈vr〉4π )2 + v2θ + v2ϕ ]〉 4π 〈ρ〉4π , (7) where 〈.〉”