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Extreme Horizon

Extreme Horizon

Resolving galactic disks in their cosmic environment

Orion

Orion

Molecular cloud fragmentation and evolution, formation of prestellar cores

Fragdisk

Fragdisk

Fragmentation of self-gravitating disks

Synthetic disk populations

Synthetic disk populations

Resolving protoplanetary disks in massive protostellar clumps

Wind of HD189733

Wind of HD189733

Unveiling the magnetic link between stars and planets

Dusty collapses

Dusty collapses

Understanding the dynamics of dust during the protostellar collapse

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  2. Star formation
  3. Turbulent box and SFR
  4. Ramses 3

Acknowledgement

Project acknowledgement

How to acknowledge my project : cite Brucy+2024


Galactica database acknowledgement

If you use it in your own work, you may acknowledge the origin of the data obtained on the Galactica database like so:

This work reused datasets available on the Galactica simulations database
(http://www.galactica-simulations.eu)
                            
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NoĆ© BRUCY  

Ramses 3

AMR grid level of refinement in a cosmological simulation

The RAMSES code is a massively parallel grid-based hydrodynamical code with adaptive mesh refinement (AMR). The data structure is called a "fully threaded tree". As opposed to "patch-based AMR", cells are refined on a cell by cell basis: it is therefore called a "tree-based AMR". A very simple interface based on "Fortran namelists" can be used to specify runtime parameters. A few routines can be modified to set more complex initial or boundary conditions. The 4 main modules are:

  • the AMR module with grid refinement, parallel communications and time steping,
  • the hydro module with a second-order unsplit Godunov solver with various slope limiters and Riemann solvers,
  • the N-body module for colisionneless particles dynamics,
  • the Poisson module with a multigrid solver for the coarse grid and a Conjugate-Gradient solver on the fine grids.

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This material is Open Data