Core-collapse supernova simulations in one and two dimensions: comparison of codes and approximations

Just, Oliver; Bollig, Robert; Janka, Hans-Thomas; Obergaulinger, M.; Glas, Robert; Nagataki, Shigehiro

doi:10.1093/mnras/sty2578

Cited by 89 publications

(97 citation statements)

References 108 publications

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“…The hydrodynamics module is coupled to an energydependent radiation-transport solver for neutrinos, which is based on an FMD two-moment scheme that evolves the zeroth and first angular moments of the Boltzmann transport equation to solve for the energy density E ν and energy-flux density F i ν (with i ∈ {r, θ, φ}) of neutrinos ν (i.e., Equations (3a-b) in Just et al 2018). Both E ν and F i ν are measured in the co-moving frame of the stellar fluid.…”

Section: Simulation Setupmentioning

confidence: 99%

“…In analogy to the hydrodynamics module, we use a Godunov-type, finite-volume scheme to solve the system of hyperbolic moment equations. The neutrinomatter interactions are implemented via source terms, which couple the neutrino moment equations to the hydrodynamics equations (i.e., Equations (2a-c) in Just et al 2018). In particular, contributions of neutrino interactions enter the equations for energy (Q E ), momentum (Q M ), and electron fraction (Q N ) of the stellar matter.…”

Section: Simulation Setupmentioning

confidence: 99%

“…In particular, contributions of neutrino interactions enter the equations for energy (Q E ), momentum (Q M ), and electron fraction (Q N ) of the stellar matter. The integration of the moment equations is performed explicitly in time (with the same time stepping as for the hydrodynamics equations) for most terms except for some interaction rates, whose source terms are treated implicitly in time (for detailed explanations, see appendix A of Just et al 2018).…”

Section: Simulation Setupmentioning

confidence: 99%

“…They hypothesize that there may be an unphysically strong feedback between the axial sloshing of the standing accretion shock instability (SASI, Blondin et al 2003) and the neutrino field, leading to explosions in axisymmetric simulations with RbR+ more readily, compared to applications employing a multigroup, fully multi-dimensional two-moment transport solver. In addition, Just et al (2018) found the RbR+ approximation to be conducive to explosions in timedependent 2D CCSN simulations in particular for models that exhibit violent activity of SASI, when compared to a fully multi-dimensional two-moment transport scheme. The 2D behavior, however, turned out to be highly stochastic and very sensitive to minor variations of the applied input physics, for which reason the 2D results were hard to interpret in a clear way.…”

Section: Introductionmentioning

confidence: 99%

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Three-dimensional Core-collapse Supernova Simulations with Multidimensional Neutrino Transport Compared to the Ray-by-ray-plus Approximation

Glas

Just

Janka

et al. 2019

ApJ

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114

101

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Self-consistent, time-dependent supernova (SN) simulations in three spatial dimensions (3D) are conducted with the Aenus-Alcar code, comparing, for the first time, calculations with fully multidimensional (FMD) neutrino transport and the ray-by-ray-plus (RbR+) approximation, both based on a two-moment solver with algebraic M1 closure. We find good agreement between 3D results with FMD and RbR+ transport for both tested grid resolutions in the cases of a 20 M progenitor, which does not explode with the employed simplified set of neutrino opacities, and of an exploding 9 M model. This is in stark contrast to corresponding axisymmetric (2D) simulations, which confirm previous claims that the RbR+ approximation can foster explosions in 2D in particular in models with powerful axial sloshing of the stalled shock due to the standing accretion shock instability (SASI). However, while local and instantaneous variations of neutrino fluxes and heating rates can still be considerably higher with RbR+ transport in 3D, the time-averaged quantities are very similar to FMD results because of the absence of a fixed, artificial symmetry axis that channels the flow. Therefore, except for stochastic fluctuations, the neutrino signals and the post-bounce evolution of 3D simulations with FMD and RbR+ transport are also very similar, in particular for our calculations with the better grid resolution. Higher spatial resolution has clearly a more important impact than the differences by the two transport treatments. Our results back up the use of the RbR+ approximation for neutrino transport in 3D SN modeling.

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Section: Simulation Setupmentioning

confidence: 99%

Section: Simulation Setupmentioning

confidence: 99%

Section: Simulation Setupmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Three-dimensional Core-collapse Supernova Simulations with Multidimensional Neutrino Transport Compared to the Ray-by-ray-plus Approximation

Glas

Just

Janka

et al. 2019

ApJ

Self Cite

114

101

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show abstract

“…On the other hand, other state-of-the-art numerical simulations have employed some approximations for neutrino transport (see e.g., (Lentz et al 2015;Takiwaki et al 2016;Kuroda et al 2016;Roberts et al 2016;Bruenn et al 2016;Pan et al 2016;Müller et al 2017;Just et al 2018;O'Connor & Couch 2018;Pan et al 2018;Glas et al 2018;Kuroda et al 2018;Vartanyan et al 2019) ). Most of them take advantage of (angular) moment approaches one way or another.…”

Section: Introductionmentioning

confidence: 99%

Three-dimensional Boltzmann-hydro Code for Core-collapse in Massive Stars. III. A New Method for Momentum Feedback from Neutrino to Matter

Nagakura

Sumiyoshi

Yamada

2019

ApJ

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We present a new method for neutrino-matter coupling in multi-dimensional radiation-hydrodynamic simulations of core-collapse supernova (CCSN) with the full Boltzmann neutrino transport. The development is motivated by the fact that the accurate conservation of momentum is required for reliable numerical modelings of CCSN dynamics including a recoil of proto-neutron star (PNS). The new method is built on a hybrid approach, in which we use the energymomentum tensor of neutrinos to compute the momentum feedback from neutrino to matter in the optically thick region while we employ the collision term in the optically thin region. In this method we utilize a general relativistic description of radiation-hydrodynamics with angular moments, which allows us to evaluate the momentum feedback from neutrino to matter without inconsistency with our Boltzmann solver. We demonstrate that the new method substantially improves the accuracy of linear momentum conservation in our CCSN simulations under reasonable angular resolutions in momentum space, alleviating the difficulty in giving the diffusion limit precisely with the discrete ordinate (S n ) method. It is the first-ever demonstration that the PNS kick can be handled directly and properly in multi-dimensional radiation-hydrodynamic simulations with the full Boltzmann neutrino transport.

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Physical, numerical, and computational challenges of modeling neutrino transport in core-collapse supernovae

Mezzacappa

Endeve

Messer

2020

Living Rev Comput Astrophys

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The proposal that core collapse supernovae are neutrino driven is still the subject of active investigation more than 50 years after the seminal paper by Colgate and White. The modern version of this paradigm, which we owe to Wilson, proposes that the supernova shock wave is powered by neutrino heating, mediated by the absorption of electron-flavor neutrinos and antineutrinos emanating from the proto-neutron star surface, or neutrinosphere. Neutrino weak interactions with the stellar core fluid, the theory of which is still evolving, are flavor and energy dependent. The associated neutrino mean free paths extend over many orders of magnitude and are never always small relative to the stellar core radius. Thus, neutrinos are never always fluid like. Instead, a kinetic description of them in terms of distribution functions that determine the number density of neutrinos in the six-dimensional phase space of position, direction, and energy, for both neutrinos and antineutrinos of each flavor, or in terms of angular moments of these neutrino distributions that instead provide neutrino number densities in the four-dimensional phase-space subspace of position and energy, is needed. In turn, the computational challenge is twofold: (i) to map the kinetic equations governing the evolution of these distributions or moments onto discrete representations that are stable, accurate, and, perhaps most important, respect physical laws such as conservation of lepton number and energy and the Fermi–Dirac nature of neutrinos and (ii) to develop efficient, supercomputer-architecture-aware solution methods for the resultant nonlinear algebraic equations. In this review, we present the current state of the art in attempts to meet this challenge.

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Core-collapse supernova simulations in one and two dimensions: comparison of codes and approximations

Cited by 89 publications

References 108 publications

Three-dimensional Core-collapse Supernova Simulations with Multidimensional Neutrino Transport Compared to the Ray-by-ray-plus Approximation

Three-dimensional Core-collapse Supernova Simulations with Multidimensional Neutrino Transport Compared to the Ray-by-ray-plus Approximation

Three-dimensional Boltzmann-hydro Code for Core-collapse in Massive Stars. III. A New Method for Momentum Feedback from Neutrino to Matter

Physical, numerical, and computational challenges of modeling neutrino transport in core-collapse supernovae

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