Accrete is a physical simulation of solar system planet formation. This simulation works by modelling a dust cloud around a Sun-like star, injecting a series of masses which collect dust, and form planets by accretion.
The Art of Computational Science: A series of books on how to build a computational lab.
AP3M is adaptive particle-particle, particle-mesh code. Older than Hydra but faster and more memory-efficient for dark-matter only calculations.
Astrolabe is a collection of subroutines and applications for calculating the positions of the sun, moon, planets and other celestial objects. The emphasis is on high accuracy over a several thousand year time span.
Cloudy is designed to simulate emission line regions.
cosmix is a celestial mechanics simulation.
Enzo is an adaptive mesh refinement (AMR), grid-based hybrid code (hydro + N-Body) which is designed to do simulations of cosmological structure formation. It uses the algorithms of Berger & Collela to improve spatial and temporal resolution in regions of large gradients, such as gravitationally collapsing objects.
FLASH is a modular, adaptive, parallel simulation code capable
of handling general compressible flow problems in astrophysical environments.
GADGET is a freely available 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.
This is a software package for generating N-body realizations of axisymmetric galaxy models consisting of disk, bulge and halo.
Gravit is a gravity simulator. It uses simple Newtonian physics using the Barnes-Hut N-body algorithm. Although the main goal of Gravit is to be as accurate as possible, it also creates beautiful looking gravity patterns. It records the history of each particle so that it can animate and display a path of its travels. At any stage you can rotate your view in 3D and zoom in and out. Gravit uses OpenGL with SDL, SDL_ttf, and SDL_image.
gyrfalcON stands for "GalaxY simulatoR using falcON". It is a full-fledged N-body code using Walter Dehnen's force algorithm of complexity O(N) (falcON), which is about 10 times faster than an optimally coded tree code. gyrfalcON features individual adaptive time steps and individual (but fixed) softening lengths.
The HNBody (Hierarchical N-Body) package integrates the motion of particles in self-gravitating systems where the total mass is dominated by a single object; it is based on symplectic integration techniques in which two-body Keplerian motion is integrated exactly. Options include choices of coordinate system, division of particles into classes based on mass scales, order of accuracy, and others.
Hydra is an adaptive particle-particle, particle-mesh plus smoothed particle hydrodynamics code.
MLAPM is a freely available code for cosmological simulations. MLAPM is purely grid-based and uses an arbitrary number of particles (each having its individual mass). The interparticle forces due to gravitational interactions are computed by solving Poisson's equation on a hierarchy of grids via Brandt's Multi-Grid algorithm.
N-Body is a set of FORTRAN codes which describe numerical simulations of many-body (N-body) gravitational interactions.
NBODY6++ provides direct N-body simulations of collisional star clusters (globulars, young dense, around galactic central black holes).
NEMO is an extendible Stellar Dynamics Toolbox, following an Open-Source Software model. It has various programs to create, integrate, analyze and visualize N-body and SPH like systems, following the pipe and filter architecture. In addition there are various tools to operate on images, tables and orbits, including FITS files to export/import to/from other astronomical data reduction packages.
OpenGLavity is a gravity simulator. It simulate gravitational interactions between N bodies with a direct N-bodies algorithm, which means that it calculates every interactions between every bodies, without any simplifications.
OrbitViewer is an interactive applet that displays the orbit of small bodies (comets or asteroids) in the solar system in 3D. The orbit may be played forwards or backwards like a movie.
Planets is a simple interactive program for playing with simulations of planetary systems, released under the GPL. It runs on Linux and Windows, and could doubtless be ported to your favorite flavor of Unix.
PMcode is Particle-Mesh code for cosmological simulations. The package allows you to simulate models with numerous combinations of parameters: open/flat/closed background, with or without the cosmological constant, different values of the Hubble constant, with or without hot neutrinos, tilted or non-tilted initial spectra, different amount of baryons.
PMFAST is a particle-mesh N-body code, written in Fortran 90 and aimed towards use in large-scale structure cosmological simulations. It offers support for distributed memory systems through MPI and shared memory via OpenMP. It features minimal memory overhead and communications requirements, running efficiently on commodity systems.
SaVi allows you to simulate satellite orbits and coverage, in two and three dimensions. SaVi is particularly useful for simulating satellite constellations such as Iridium and Globalstar.
Solar Visitor is a space simulator where the user flies around our solar system in a 3D view; the planets move too. It uses the Ogre graphics library, and accelerated OpenGL is highly recommended.
StarCrash is a parallel fortran code based on Smoothed Particle Hydrodynamics (SPH) techniques to calculate the 3-d evolution of self-gravitating fluid systems.
The code in particularly suited to the study of stellar interactions, such as mergers of binary star systems and stellar collisions.
Starlab is a software package for simulating the evolution of dense stellar systems and analyzing the resultant data. It is a collection of loosely coupled programs (tools) linked at the level of the UNIX operating system. The tools share a common data structure and can be combined in arbitrarily complex ways to study the dynamics of star clusters and galactic nuclei.
The SWIFT subroutine package is designed to integrate a set of mutually gravitationally interacting bodies together with a group of test particles which feel the gravitational influence of the massive bodies but do not affect each other or the massive bodies.
TPM is a code for carrying out collisionless (dark matter) cosmological N-body simulations, evolving a system of N particles as they move under their mutual gravitational interaction. It combines aspects of both Tree and Particle-Mesh algorithms. The code is parallel and uses MPI for message passing.
XGrav is a simple physics simulation for a large number of particles. It simulates
the effect of gravity, collisions, heat dissipation and a simple chemical reaction.
The simulation is in no way meant to be realistic but rather a toy with which you
can create stars, planets and even simple solar systems.
XStar simulates the movement of stars. It starts by putting a bunch of stars on the screen, and then it lets the inter-body gravitational forces move the stars around. The result is a lot of neat wandering paths, as the stars interact and collide.
Zeus-MP is a parallel, Eulerian (grid-based) MHD code for use in astronomical simulations. It freely available and is written in FORTRAN 77. It is primarily intended for workstations and Beowulf clusters. This is a modified version of the initial NCSA release.