FLASH: An Adaptive Mesh Hydrodynamics Code for Modeling Astrophysical Thermonuclear Flashes

By B. Fryxell, K. Olson, Paul M. Ricker, Francis Timmes, Michael Zingale, D. Lamb, P. MacNeice, R. Rosner, J. Truran, H. Tufo. 2000

2,230 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a6beab31174a8e48aca051d6711de3160e2745cc

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Citations in the corpus

Turbulent Structure of a Stratified Supernova-driven Interstellar Medium (2005, methodology): “The software used in this work was in part developed by the DOE-supported ASCI/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago.”
The Density Probability Distribution in Compressible Isothermal Turbulence: Solenoidal versus Compressive Forcing (2008, methodology): “The piecewise parabolic method (Colella & Woodward 1984) implementation of FLASH3 (Fryxell et al. 2000; Dubey et al. 2008) was used to solve the hydrodynamic equations on periodic uniform grids with 163841, 40962, and 10243 grid points in 1, 2 and 3 dimension(s) (1D, 2D, 3D).”
The Athena++ Adaptive Mesh Refinement Framework: Design and Magnetohydrodynamic Solvers (2020, methodology): “For comparison, we have run the same benchmark problem using the same algorithmic choices and the same compiler optimizations for the latest public versions of the FLASH, PLUTO, and Enzo codes, and we find that the per-core performance of Athena++ is the highest of all four, in some cases by as much”
SEEING THE COLLISION OF A SUPERNOVA WITH ITS COMPANION STAR (2009, methodology): “Figure 1 illustrates the hydrodynamics of the interaction in a 2-dimensional numerical calculation using the FLASH code (Fryxell et al. 2000) and assuming a polytropic γ = 4/3 equation of state, appropriate for a radiation dominated gas.”
On the universality of supersonic turbulence (2013, methodology): “We use the FLASH code (Fryxell et al. 2000; Dubey et al. 2008) in its current version (v4) to solve the compressible gas-dynamical equations on three-dimensional, uniform, periodic grids of fixed side length L with resolutions of 2563, 5123, 10243, 20483 and 40963 grid points.”
AN AMR STUDY OF THE COMMON-ENVELOPE PHASE OF BINARY EVOLUTION (2011, methodology): “We linearly interpolate this model onto a 3D Eulerian mesh for use in the FLASH 2.4 adaptive mesh refinement (AMR) simulation code (Fryxell et al. 2000).”
Type Ia Supernova Explosion: Gravitationally Confined Detonation (2004, methodology): “The simulations presented here were performed with the adaptive mesh refinement hydrodynamics code flash (Fryxell et al. 2000).”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, methodology): “…of selected simulation data see the SILCC website: www.astro.uni-koeln.de/silcc c© 0000 RAS, MNRAS 000, 000–000 out with the astrophysical code FLASH in version 4 (Fryxell et al. 2000; Dubey et al. 2008, 2013), which is an adaptive mesh refinement (AMR) code developed at the University of Chicago.”
MODELING COLLAPSE AND ACCRETION IN TURBULENT GAS CLOUDS: IMPLEMENTATION AND COMPARISON OF SINK PARTICLES IN AMR AND SPH (2010, methodology): “The Basic flash Code The flash code3 (Fryxell et al. 2000; Dubey et al. 2008) is an adaptive mesh refinement (amr) code (Berger & Colella 1989).”
Cosmological radiative transfer codes comparison project – I. The static density field tests (2006, positive): “The process of making a dynamic coupling of SIMPLEX with the grid-based hydrocodes FLASH (Fryxell et al. 2000) and GADGET-2 (Springel 2005) is under way.”
MHD simulations of jet acceleration from Keplerian accretion disks - The effects of disk resistivity (2007, methodology): “(1)–(4), we employ a modified version of the MHD module provided with the public code FLASH1 (Fryxell et al. 2000) developed at the ASC FLASH Center at the University of Chicago, adopting its AMR capabilities.”
THE INTERPLAY OF MAGNETIC FIELDS, FRAGMENTATION, AND IONIZATION FEEDBACK IN HIGH-MASS STAR FORMATION (2010, neutral): “The FLASH code was in part developed by the DOE-supported Alliances Center for Astrophysical Thermonuclear Flashes (ASCI) at the University of Chicago.”
Numerical Methods for Evolutionary Differential Equations (2008, background): “We shall not dwell on this much here; see Monaghan [136] for a recent, long review of these methods (which originated in the 1970s) and [64] for a large state-of-the-art hydrodynamic code implementing it for astrophysical purposes.”
Global comparison of core-collapse supernova simulations in spherical symmetry (2018, background): “Recently [16] have implemented both a general relativistic effective potential [21] and a twomoment, energy-dependent neutrino transport scheme into FLASH following closely the implementation of [55] (also see the code description for GR1D below).”
The SILCC project - III. Regulation of star formation and outflows by stellar winds and supernovae (2016, methodology): “2 N U M E R I C A L M E T H O D We use the Eulerian, adaptive mesh refinement, MHD code FLASH 4 (Fryxell et al. 2000; Dubey et al. 2008, 2013) with the directionally split, Bouchut HLL5R solver (Bouchut, Klingenberg & Waagan 2007, 2010; Waagan 2009; Waagan, Federrath & Klingenberg 2011) to simulate…”
LIMITING ACCRETION ONTO MASSIVE STARS BY FRAGMENTATION-INDUCED STARVATION (2010, methodology): “The FLASH code was in part developed by the DOE-supported Alliances Center for Astrophysical Thermonuclear Flashes (ASCI) at the University of Chicago.”
THE GENERATION OF STRONG MAGNETIC FIELDS DURING THE FORMATION OF THE FIRST STARS (2010, neutral): “5 (Fryxell et al. 2000).”
CASTRO: A NEW COMPRESSIBLE ASTROPHYSICAL SOLVER. I. HYDRODYNAMICS AND SELF-GRAVITY (2010, methodology): “A standard approach (see for example Fryxell et al. 2000; Omang et al. 2006 and the references therein) is to convert the explosion energy into a pressure contained within a certain volume, Vinit, of radius rinit as pinit = (γ − 1)Eexp Vinit .”
SURFACE DETONATIONS IN DOUBLE DEGENERATE BINARY SYSTEMS TRIGGERED BY ACCRETION STREAM INSTABILITIES (2009, methodology): “We follow the impact of the mass transfer onto the orbital evolution by performing an SPH simulation (Dan et al. 2009, in prep.) and use the obtained, time-dependent results for orbital separation andṀ as boundary conditions for FLASH (Fryxell et al. 2000).”