Commission B1 Computational Astrophysics

Agama is a software package for stellar dynamics, providing tools for working with gravitational potentials, orbits, action-angle coordinates, distribution functions, self-consistent models and more.

Arepo is a massively parallel gravity and magnetohydrodynamics code for astrophysics, designed for problems of large dynamic range. It employs a finite-volume approach to discretize the equations of hydrodynamics on a moving Voronoi mesh, and a tree-particle-mesh method for gravitational interactions. Arepo is originally optimized for cosmological simulations of structure formation, but has also been used in many other applications in astrophysics.

AstroBEAR is a parallelized hydrodynamic/MHD simulation code suitable for a variety of astrophysical problems. Derived from the BearCLAW package written by Sorin Mitran, AstroBEAR is designed for 2D and 3D adaptive mesh refinement (AMR), multiphysics simulations.

Grid-based adaptive mesh refinement (AMR) code for hydrodynamics, magnetohydrodynamics (MHD), and special and general relativistic MHD including other physics such as particles, self-gravity, chemistry, and radiation transport.

BHAC (the Black Hole Accretion Code) is a multidimensional general relativistic magnetohydrodynamics code based on the MPI-AMRVAC framework. BHAC solves the equations of ideal general relativistic magnetohydrodynamics in one, two or three dimensions on arbitrary stationary space-times, using an efficient block based adaptive mesh refinement approach.

GAMER is a GPU-accelerated adaptive mesh refinement code for astrophysics. It features extremely high performance and parallel scalability and supports a rich set of physics modules, including hydrodynamics, MHD, self-gravity, particles, chemistry, radiative processes, and wave (fuzzy) dark matter.

GADGET is a code for cosmological N-body/SPH simulations on massively parallel computers with distributed memory. GADGET uses an explicit communication model that is implemented with the standardized MPI communication interface. The code can be run on essentially all supercomputer systems presently in use, including clusters of workstations or individual PCs. GADGET computes gravitational forces with a hierarchical tree algorithm (optionally in combination with a particle-mesh scheme for long-range gravitational forces) and represents fluids by means of smoothed particle hydrodynamics (SPH). The code can be used for studies of isolated systems, or for simulations that include the cosmological expansion of space, both with or without periodic boundary conditions. In all these types of simulations, GADGET follows the evolution of a self-gravitating collisionless N-body system, and allows gas dynamics to be optionally included. Both the force computation and the time stepping of GADGET are fully adaptive. GADGET can therefore be used to address a wide array of astrophysically interesting problems, ranging from colliding and merging galaxies, to the formation of large-scale structure in the Universe. With the inclusion of additional physical processes such as radiative cooling and heating, GADGET can also be used to study the dynamics of the gaseous intergalactic medium, or to address star formation and its regulation by feedback processes.

GIZMO is a flexible, massively-parallel, multi-physics simulation code. The code lets you solve the fluid equations using a variety of different methods -- whatever is best for the problem at hand. It introduces new Lagrangian Godunov-type methods that allow you to solve the fluid equations with a moving particle distribution that is automatically adaptive in resolution and avoids the advection errors, angular momentum conservation errors, and excessive diffusion problems that limit the applicability of “adaptive mesh” (AMR) codes, while simultaneously avoiding the low-order errors inherent to simpler methods like smoothed-particle hydrodynamics (SPH). Meanwhile, self-gravity is solved fast, with fully-adaptive gravitational softenings. And the code is massively parallel — it has been run on everything from a Mac laptop to > 1 million CPUs on national supercomputers. It includes a variety of physics including magnetohydrodynamics, self-gravity, cosmology, radiative heating/cooling, radiation-hydrodynamics, sink particles, star and black hole formation and “feedback”, anisotropic conduction and viscosity, turbulent eddy diffusion, dust/particulate dynamics, non-standard dark matter and dark energy models, elastic and plastic dynamics, giant impact/material models, shearing boxes and large-eddy/driven-turbulent boxes, and more.

GR MHD code to simulate black hole accretion with optional nuclear Equation of State and neutrino cooling. MPI-parallelized, 3D simulation of accretion and jet ejection in the Kerr metric around rotating black hole, in case of the gamma-ray burst engine, is its main application.

The code was built upon the HARM-2D General Relativistic scheme for magneto-hydrodynamical simulations for black hole accretion (Gammie et al. 2003). It was extensively upgraded and supplied with novel functionality. The EOS functions are computed for the Fermi Gas of free proton, neutron, electron-positron, under arbitrary degeneracy (Yuan 2005). Tables with the equation of state and neutrino cooling are tabulated in the function of temperature and density and dynamically stored during the simulation. The physical units adopted in the code are scaled with the black hole mass and density scale in the accretion disk. The interpolation over EOS tables is implemented within the conversion scheme between conserved and primitive variables in GR MHD solver. In addition, code makes use of the tracer particles, and stores output on them for the subsequent post-processing of the r-process nucleosynthesis. Output formats in current version are ASCII and HDF5.

This version, as of 2020, was developed since 2012, by Agnieszka Janiuk, Ireneusz Janiuk, and Kostas Sapountzis. From our website one can download .zip with sources, sample initail condition, and sample makefile. One can find there also the README file with technical details.

A performance portable version (using Kokkos ) of Athena++ for structured grid (magnetohydro)dynamics simulations on any architecture (CPUs, KNLs, GPUs, ...)

Legolas is a finite element code for MHD spectroscopy of 1D Cartesian/cylindrical equilibria with flow that balance pressure gradients, gravity and Lorentz forces, enriched with various non-adiabatic effects. The code’s capabilities range from full spectrum calculations to investigating eigenfunctions of specific modes to full-on parametric studies of various equilibrium configurations.

A generic tool for block-grid-adaptive simulations of your favourite system of PDEs, in any dimensionality. This includes hydro, MHD, reaction-diffusion, ...)

This code is designed to simulate large collisional N-body systems (star clusters), including the accurate treatment of binary and few-body dynamics. The single and binary stellar evolutions codes, SSE/BSE, are implemented. The time-evolving external tidal fields based on tidal tensor methods are imported from NBODY6TT as an optional package.

Phantom is a 3D Smoothed Particle Hydrodynamics and Magnetohydrodynamics code for astrophysics. It was written and developed by Daniel Price with contributions from many others. It is designed to be a fast 3D SPH code with a low memory footprint, for production runs. Physics includes hydro, MHD, multigrain dust, self-gravity and sink particles.

PION is a grid-based fluid dynamics code for hydrodynamics and magnetohydrodynamics, including a ray-tracing module for calculating the attenuation of radiation from point sources of ionizing photons. It also has a module for coupling fluid dynamics and the radiation field to microphysical processes such as heating/cooling and ionization/recombination. PION was written to model the evolution of HII regions, photoionized bubbles that form around hot stars, and developed to include stellar wind sources so that both wind bubbles and photoionized bubbles can be simulated at the same time. Static mesh-refinement is implemented and PION is parallelised with MPI for running on distributed-memory machines. Active development of new features takes place mostly on a private branch of the git repository and prospective developers are advised to contact info@pion.ie before starting development work on the released source code.

PLUTO is a freely-distributed software for the numerical solution of mixed hyperbolic/parabolic systems of partial differential equations (conservation laws) targeting high Mach number flows in astrophysical fluid dynamics. The code is designed with a modular and flexible structure whereby different numerical algorithms can be separately combined to solve systems of conservation laws using the finite volume or finite difference approach based on Godunov-type schemes.

The code is written in the C programming language while the AMR interface also requires also C++ and Fortran. The current release adds Particles support, Hall MHD, forced turbulence and RK-Legendre time stepping for parabolic problems.

RADMC-3D is a highly flexible diagnostic radiative transfer code for "postprocessing" models to compute predictions for observable images and spectra. It is not a "model" itself, but a code with which the observational appearance of models can be computed. These "input models" can be e.g. the results from hydrodynamic simulations or parameterized density distributions. Typical applications are protoplanetary disks, AGN tori, molecular clouds, ISM turbulence etc.

RAMSES is an open source code to model astrophysical systems, featuring self-gravitating, magnetised, compressible, radiative fluid flows. It is based on the Adaptive Mesh Refinement (AMR) technique on a fully-threaded graded octree. RAMSES is written in Fortran 90 and is making intensive use of the Message Passing Interface (MPI) library.

REBOUND is an N-body integrator, i.e. a software package that can integrate the motion of particles under the influence of gravity. The particles can represent stars, planets, moons, ring or dust particles. REBOUND is very flexible and can be customized to accurately and efficiently solve many problems in astrophysics.