NEMO
[open source - Unix] An extendible stellar dynamics toolbox; has various programs to create, integrate, analyze and visualize N-body and SPH-like systems. 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.
COSMOMC-- Monte Carlo evaluation of CMB parameters
COSMOMC calculates a fast Markov Chain Monte-Carlo exploration of cosmological parameter space for an input set of constraints.
Enzo
Enzo is an adaptive mesh refinement (AMR), grid-based hybrid code (hydro + N-Body) which is designed to do simulations of cosmological structure formation.
FLASH -- AMR reacting hydrodynamics
The FLASH code is a reacting hydrodynamics code with adaptive mesh refinement for general astrophysical hydrodynamics problems.
A TIPSY file viewer with MPI capabilities
[Open source - Linux] "Hubble in a bottle!" is visualization software for N-body simulations, which can be run in parallel using MPI for visualizing very large simulation results. Simulation output must be in TIPSY format.
CFD codes list
A large list of commercial, public-domain and shareware Computational Fluid Dynamics codes.
ZEUS-MP Version 2
ZEUS is a venerable astrophysical hydrodynamics and MHD code that has been used to investigate a wide variety of astrophysical problems. The latest version includes gas hydrodynamics, ideal MHD, implicit flux-limited radiation diffusion (FLD), self gravity, and multispecies advection.
ORSA - Orbit Reconstruction, Simulation and Analysis
ORSA is a C++ framework for the development of algorithms and programs oriented to the simulation and analysis of the orbital evolution of bodies in space.
Stellar Astrophysics Software
[open source - Windows] Various programs for stellar astrophysics. Includes CHANDRA stellar structure software for collapsed objects including rotating white dwarfs and neutron stars, and STARCAL for nuclear astrophysics and the stellar structure of main sequence stars with supernova forecasting.
N-Body/Particle Simulation Methods
An extensive online tutorial with examples and code references.
The Art of Computational Science
An online `socratic book' pedagogically describing the building of a N-body simulation code for stellar systems. Software (in Ruby) is included.
Aarseth's N-body software
[open source - multiplatform] Direct N-body algorithms.
CMBEASY -- CMB calculations with Graphical User Interface
CMBEASY is a C++ code with GUI for calculation of CMB power spectra and other density fluctuation evolution data for a given cosmology.
PHOEBE (PHysics Of Eclipsing BinariEs)
PHOEBE is an infrastructure for the numerical modeling and analysis of eclipsing binary stars, using a variety of models.
CAPGADGET
[open source - multiplatform] Visualization package to capture and display Gadget N-body simulations.
Barnes & Hut Treecode Algorithm
[open source - multiplatform] A guide to a tree code algorithm implementation, used for astronomical N-body simulations.
EZ Stellar Evolution
EZ (Evolve ZAMS) Stellar Evolution tracks the evolution of new (Zero-Age Main Sequence) stars throughout the bulk of their lives (until an event which EZ does not model occurs, such as a Helium Flash or core crystallization). The code is clean and well documented. Links include a web interface to the code.
Gadget-2
The Gadget-2 code is an SPH simulation code designed for cosmological simulations but can be used for a wide variety of astrophysical hydrodynamics simulations with self-gravity.
Cloudy & Associates - Photoionization simulations for the discriminating astrophysicist
Cloudy is an extensive, well-established, large-scale spectral synthesis code designed to simulate fully physical conditions within an astronomical plasma and then predict the emitted spectrum. The web page contains links to papers published with cloudy, the most recent version of the software itself, and a discussion board.
DUSTY -- Radiation transfer through dust
DUSTY calculates the emerging spectrum of radiation from some source viewed after processing by a dusty region. The original radiation is scattered, absorbed and reemitted by the dust, and the emerging processed spectrum often provides the only available information about the embedded object. DUSTY can handle both planar and centrally-heated spherical density distributions. The number of independent input model parameters is minimized by fully implementing the scaling properties of the radiative transfer problem, and the spatial temperature profile is found from radiative equilibrium at every point in the dusty region. DUSTY has built in optical properties for the most common types of astronomical dust and comes with a library for many other grains.
|