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Resolving galactic disks in their cosmic environment

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Molecular cloud fragmentation and evolution, formation of prestellar cores

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Understanding the dynamics of dust during the protostellar collapse

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Acknowledgement

Project acknowledgement

You may acknowledge this project by citing the associated paper Brucy & Hennebelle 2021.

@ARTICLE{2021MNRAS.503.4192B,
       author = {{Brucy}, No{\'e} and {Hennebelle}, Patrick},
        title = "{A two-step gravitational cascade for the fragmentation of self-gravitating discs}",
      journal = {\mnras},
     keywords = {accretion, accretion discs, gravitation, hydrodynamics, instabilities, methods: numerical, protoplanetary discs, Astrophysics - Astrophysics of Galaxies, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics},
         year = 2021,
        month = may,
       volume = {503},
       number = {3},
        pages = {4192-4207},
          doi = {10.1093/mnras/stab738},
archivePrefix = {arXiv},
       eprint = {2103.05508},
 primaryClass = {astro-ph.GA},
       adsurl = {https://ui.adsabs.harvard.edu/abs/2021MNRAS.503.4192B},
      adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

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)
Cite me
Noé BRUCY  

beta8_jr13_tic

  • Summary
  • Parameters
  • Snapshots
    • t=$4.91559$

Summary

Group jr13_tic, $\beta = 8.0$.

Simulated using Ramses 3 (MHD)

Parameters

Parameter Value
lmin 6
lmax 13
$\beta$ 8
tic

Snapshots

'130' snapshot datafile download

Select the datafiles you wish to export from this snapshot (a zip file containing the requested datafiles will be prepared) :

130 (t=$4.91559$)

Snapshot at 4.92 ORPs.

Notations:

$r_d$ : radius of the disk
ORP : outer rotation period, that is period of the gas at $r_d$
$M_\star$ : Mass of the central object
$v_{k,d}$ : Keplerian speed at $r_d$

All slices are taken at $z=0$ or $y=0$.

Datafiles:
coldens_z
Column density map (z)
  • HDF5 
  • JPEG 
coldens_y
Column density map (y)
  • HDF5 
  • JPEG 
slice_rho_z
Density slice (z)
  • HDF5 
  • JPEG 
slice_rho_y
Density slice (y)
  • HDF5 
  • JPEG 
slice_P_z
Pressure slice (z)
  • HDF5 
  • JPEG 
slice_velr_z
Radial velocity slice (z)
  • HDF5 
  • JPEG 
slice_velphi_z
Orthoradial velocity slice (z)
  • HDF5 
  • JPEG 
pdf_coldens_z
Probability function of the logarithm of the column density fluctuations $\sigma = \Sigma/\overline{\Sigma}$ with respect to its azimuthal average (z)
  • HDF5 
  • JPEG 

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This material is Open Data