Chimera: A Massively Parallel Code for Core-collapse Supernova Simulations

Blondin, John M.; Hix, W. R.; Lentz, Eric J.; Messer, O. E. Bronson; Mezzacappa, Anthony; Endeve, Eirik; Harris, J. Austin; Marronetti, Pedro; Budiardja, Reuben D.; Chertkow, Merek A.; Lee, Ching-Tsai

doi:10.3847/1538-4365/ab7aff

Cited by 54 publications

(43 citation statements)

References 91 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Nowadays, the vast majority of codes use Godunov-based high-resolution shock capturing (HRSC) schemes with higher-order reconstruction (see, e.g., LeVeque 1998b; Martí and Müller 2015; Balsara 2017 for a thorough introduction). Examples include implementations of the piecewise parabolic method of Colella and Glaz (1985) or extensions thereof in the Newtonian hydroydnamics codes PROMETHEUS (Fryxell et al 1989(Fryxell et al , 1991Müller et al 1991), which has been integrated into various neutrino transport solvers by the Garching group (Rampp and Janka 2002;Buras et al 2006b;Scheck et al 2006), its offshoot PROMPI (Meakin and Arnett 2007b), PPMSTAR (Woodward et al 2019), VH1 (Blondin and Lufkin 1993;Hawley et al 2012) as used within the CHIMERA transport code (Bruenn et al 2018), FLASH (Fryxell et al 2000), CASTRO (Almgren et al 2006), ALCAR (Just et al 2015), and FORNAX (Skinner et al 2019). This approach is also used in most general relativistic (GR) hydrodynamics codes for core-collapse supernovae like COCONUT (Dimmelmeier et al 2002;Müller et al 2010), ZELMANI (Reisswig et al 2013;Roberts et al 2016), and GRHYDRO (Mösta et al 2014a).…”

Section: Hydrodynamicsmentioning

confidence: 99%

“…In spherical coordinates, the multi-scale nature of the problem can be accommodated to a large degree by employing a non-uniform radial grid that transitions to roughly equal spacing in log r at large radii. Radial resolution can be added selectively in strongly stratified regions like the PNS surface (Buras et al 2006b), or one can use an adaptive moving radial grid (Liebendörfer et al 2004;Bruenn et al 2018). However, some care must be exercised in using non-uniform radial grids.…”

Section: Problem Geometry and Choice Of Gridsmentioning

confidence: 99%

“…The MPA/Monash group routinely apply such a moving radial grid in quasi-Lagrangian mode during the collapse phase (Rampp and Janka 2000), and, with a prescribed grid function, in parameterized multi-D simulations of neutrino-driven explosions (Janka and Müller 1996;Scheck et al 2006) and in simulations of convective burning (Müller et al 2016b). The Oak Ridge group uses a truly adaptive radial grid in their supernova simulations with the CHIMERA code (Bruenn et al 2018). A moving radial mesh might also appear useful for following the expansion of the ejecta and the formation of a strongly diluted central region in simulations of mixing instabilities in the envelope, but the definition of an appropriate grid function is nontrivial.…”

Section: Problem Geometry and Choice Of Gridsmentioning

confidence: 99%

See 2 more Smart Citations

Hydrodynamics of core-collapse supernovae and their progenitors

Müller¹

2020

Living Rev Comput Astrophys

148

View full text Add to dashboard Cite

Multi-dimensional fluid flow plays a paramount role in the explosions of massive stars as core-collapse supernovae. In recent years, three-dimensional (3D) simulations of these phenomena have matured significantly. Considerable progress has been made towards identifying the ingredients for shock revival by the neutrino-driven mechanism, and successful explosions have already been obtained in a number of selfconsistent 3D models. These advances also bring new challenges, however. Prompted by a need for increased physical realism and meaningful model validation, supernova theory is now moving towards a more integrated view that connects multi-dimensional phenomena in the late convective burning stages prior to collapse, the explosion engine, and mixing instabilities in the supernova envelope. Here we review our current understanding of multi-D fluid flow in core-collapse supernovae and their progenitors. We start by outlining specific challenges faced by hydrodynamic simulations of core-collapse supernovae and of the late convective burning stages. We then discuss recent advances and open questions in theory and simulations.

show abstract

Section: Hydrodynamicsmentioning

confidence: 99%

Section: Problem Geometry and Choice Of Gridsmentioning

confidence: 99%

Section: Problem Geometry and Choice Of Gridsmentioning

confidence: 99%

See 1 more Smart Citation

Hydrodynamics of core-collapse supernovae and their progenitors

Müller¹

2020

Living Rev Comput Astrophys

148

View full text Add to dashboard Cite

show abstract

“…In the end, such approximations must be removed, if only just to check them. The rayby-ray approach of the Oak Ridge group is based on one-moment closure through flux-limited diffusion (Bruenn et al 2020). They follow the evolution for the lowest angular moment of the neutrino distribution: the number density.…”

Section: Setting the Stagementioning

confidence: 99%

“…One-moment models [commonly referred to as flux-limited diffusion models (Levermore and Pomraning 1981)] are among the earliest transport models adopted for neutrino transport in core-collapse supernova simulations (Bruenn 1975), and are still in use today (e.g., Bruenn et al 2020;Rahman et al 2019). Essentially, one-moment models evolve only the zeroth moment of the distribution function, while higher-order moments are specified through a closure procedure.…”

Section: One-moment Kineticsmentioning

confidence: 99%

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

Mezzacappa

Endeve

Messer

2020

Living Rev Comput Astrophys

Self Cite

View full text Add to dashboard Cite

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.

show abstract