Simulating Radiating and Magnetized Flows in Multiple Dimensions with ZEUS-MP

By John C. Hayes, M. Norman, Robert A. Fiedler, James Bordner, P. Li, S. E. Clark, A. ud-Doula, M. Mac Low. 2005

283 citations recorded by the source corpus.

This paper describes ZEUS-MP, a multiphysics, massively parallel, message-passing implementation of the ZEUS code. ZEUS-MP differs significantly from the thoroughly documented ZEUS-2D code, the completely undocumented (in peer-reviewed literature) ZEUS-3D code, and a marginally documented "version 1" of ZEUS-MP first distributed publicly in 1999. ZEUS-MP offers an MHD algorithm that is better suited for multidimensional flows than the ZEUS-2D module by virtue of modifications to the method of characteristics scheme first suggested by Hawley & Stone. This MHD module is shown to compare quite favorably to the TVD scheme described by Ryu et al. ZEUS-MP is the first publicly available ZEUS code to allow the advection of multiple chemical (or nuclear) species. Radiation hydrodynamic simulations are enabled via an implicit flux-limited radiation diffusion (FLD) module. The hydrodynamic, MHD, and FLD modules can be used, singly or in concert, in one, two, or three space dimensions. In addition, so-called 1.5D and 2.5D grids, in which the "half-D" denotes a symmetry axis along which a constant but nonzero value of velocity or magnetic field is evolved, are supported. Self-gravity can be included either through the assumption of a GM/r potential or through a solution of Poisson's equation using one of three linear solver packages (conjugate gradient, multigrid, and FFT) provided for that purpose. Point-mass potentials are also supported. Because ZEUS-MP is designed for large simulations on parallel computing platforms, considerable attention is paid to the parallel performance characteristics of each module in the code. Strong-scaling tests involving pure hydrodynamics (with and without self-gravity), MHD, and RHD are performed in which large problems (2563 zones) are distributed among as many as 1024 processors of an IBM SP3. Parallel efficiency is a strong function of the amount of communication required between processors in a given algorithm, but all modules are shown to scale well on up to 1024 processors for the chosen fixed problem size.

Subfields: Aerospace Engineering, Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/ce6294071d10f30efdaa7d21a60e059041465089

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Citations in the corpus

Modelling CO formation in the turbulent interstellar medium (2009, methodology): “In testing our modified version of ZEUS-MP, our main focus was on verifying the additional physics that we have added to the code, as the unmodified code has already undergone significant testing (see e.g. Stone & Norman 1992a,b; Hayes et al. 2006).”
Population III Star Formation in a ΛCDM Universe. I. The Effect of Formation Redshift and Environment on Protostellar Accretion Rate (2006, methodology): “…this takes place at high densities, where the optically thin assumption used in the Enzo cooling algorithms breaks down, which necessitates either an extension of the cooling model (Ripamonti & Abel 2004) or the use of a radiation hydrodynamics code such as ZEUS-MP (Hayes et al. 2006).”
The density variance–Mach number relation in supersonic turbulence – I. Isothermal, magnetized gas (2012, methodology): “We have performed simulations of the evolution of the turbulent, dense, inviscid, magnetized (MHD) and unmagnetized [hydrodynamic (HD)], isothermal interstellar medium using a modified version of the ZEUS-MP hydrodynamical code (Norman 2000; Hayes et al. 2006).”
On the relationship between molecular hydrogen and carbon monoxide abundances in molecular clouds (2010, methodology): “Our simulations were performed using a modified version of the ZEUS-MPmagnetohydrodynamical code (Norman 2000; Hayes et al. 2006) fully described in Paper I.”
Athena: A New Code for Astrophysical MHD (2008, methodology): “This algorithm, as implemented in for example the ZEUS code (Stone &Norman1992a,1992b; Clarke1996; Hayes et al. 2006), has been used for many hundreds of applications in astrophysics.”
The Athena++ Adaptive Mesh Refinement Framework: Design and Magnetohydrodynamic Solvers (2020, background): “Examples of widelyused (based on, e.g., citations) grid-based codes include ZEUS (Stone & Norman 1992a,b; Stone et al. 1992; Hayes et al. 2006), ART (Kravtsov et al. 1997), FLASH (Fryxell et al. 2000), RAMSES (Teyssier 2002), HARM (Gammie et al. 2003), PLUTO (Mignone et al. 2007; Mignone et…”
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, methodology): “As for the hydro-solver, we employ the ZEUS-MP code (Hayes et al. 2006) which has been modified for core-collapse simulations (e.g., Iwakami et al. 2008, 2009).”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “A fourth group has used a version of the Zeus-MP code (Hayes et al. 2006; Iwakami et al. 2008, 2009a) for hydrodynamics and the IDSA scheme for neutrino transport (Liebendörfer et al. 2009), which we will refer to as ‘Zeus+IDSA.’”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, methodology): “Here we briefly summarize several major updates of the code that we have implemented after our previous work (Takiwaki et al. 2012) in which the spectral neutrino transport scheme IDSA (Liebendörfer et al. 2009) was implemented in the ZEUS-MP code (Hayes et al. 2006).”
The Destruction of Cosmological Minihalos by Primordial Supernovae (2008, background): “See Hayes et al. (2006) for a discussion of ZEUS-MP’s moving Eulerian grid option.”
On the theory of disc photoevaporation (2011, methodology): “The simulations were performed using a modified version of the ZEUS-MP/2 code7 (Hayes et al. 2006), the modifications of which are described in detail in Hayes et al. (2006).”
RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR COLLAPSE: PROTOSTELLAR CORE FORMATION (2012, methodology): “(37) By substituting (36) into (37), we can eliminate the equation related to gas energy (Hayes et al. 2006; this procedure corresponds to performing partial LU decomposition analytically).”
yt: A MULTI-CODE ANALYSIS TOOLKIT FOR ASTROPHYSICAL SIMULATION DATA (2010, unknown): “We also hope to work with other research groups to add support for the visualization and analysis of output from other popular astrophysics simulation codes such as ART, Gadget, Pluto (Mignone et al. 2007), and ZEUS-MP (Hayes et al. 2006).”
Thermal instability and the feedback regulation of hot haloes in clusters, groups and galaxies (2011, methodology): “We model the ICM in spherical (r, θ, φ) geometry using the ZEUS-MP code (Hayes et al. 2006).”
Validation of numerical codes for impact and explosion cratering: Impacts on strengthless and metal targets (2008, methodology): “SPH is used in 1D, 2D and 3D. ZEUS-MP2, originally built to model the behavior of gases in astrophysical situations (Hayes et al. 2006), has been modified for use in 2D and 3D Eulerian impact calculations (Korycansky et al. 2000, 2002; see Korycansky and Zahnle 2003 for the earlier version ZEUS-MP).”
Equations and Algorithms for Mixed-frame Flux-limited Diffusion Radiation Hydrodynamics (2006, methodology): “This may be done either at the same time one is iterating to update the flux divergence term ∇ · F (Whitehouse et al. 2005), or in a separate iteration to be done once the iterative solve for the flux divergence update is complete (Turner & Stone 2001; Hayes et al. 2006).”