Ramses Documentation

The ramses code is intended to be a versatile platform to develop applications using Adaptive Mesh Refinement (AMR) for computational astrophysics. The current implementation allows solving the classical and relativistic Euler equations in presence of self-gravity, magnetic field and radiation field. The ramses code can be used on massively parallel architectures, if properly linked to the MPI library. It can also be used on single processor machines without MPI. Output data are generated using Fortran unformatted files. A suite of post-processing routines is delivered within the present release, allowing the user to perform a simple analysis of the generated output files. A pdf version of this documentation can be found here.

Table of Contents

User Documentation

• Getting started
  • Obtaining the package
  • Compiling the code
  • Executing the test case
  • Reading the log file
• Runtime Parameters
  • Global parameters
  • AMR Parameters
  • Initial Conditions Parameters
  • Output Parameters
  • Boundary Parameters
  • Hydro parameters
  • Parameters
  • Poisson Parameters
  • Refinement parameters
  • Clumpfinder (PHEW)
  • Particle Unbinding
  • Making Mergertrees (And Mock Galaxies)
  • Sink particles
  • Movies
  • Turbulence driving
  • Monte Carlo tracer particles
• Cosmological simulations
  • Restart from previous output
  • Saving progress before job limit termination
  • Dump immediate output
• Advanced simulations
  • Changing the source code
  • Patch directory
  • Radiation Hydrodynamics in RAMSES
• Testing
  • 1. Running the automatic test suite
  • 2. Creating a new test
  • 3. Creating a new group of tests

Developer Documentation

• Documentation
• Acknowledgements