•  Home
  •  Topics 
    •  Solar Physics
    •  Planetary atmospheres
    •  Stellar environments
    •  Star-planet interactions
    •  Stellar physics
    •  Star formation
    •  Interstellar medium
    •  Supernovae
    •  Galactic dynamics
    •  Cosmology
  •  About Galactica
  •  Publish my projects
  •  Share massive data
  •  Log in
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

Previous Next
  1. Home
  2. Star formation
  3. LS

Acknowledgement

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
Patrick HENNEBELLE  

LS

Summary

This project aims at modelling self-consistently a piece of galaxy as described in Hennebelle & Iffrig 2014, A&A, 570, 80 and Iffrig & Hennebelle 2017, A&A, 604, 70. Computational boxes of about 1 kpc are considered. An external gravitational potential, due to the dark matter and stellar component of the galaxies is added and induce the disk stratification. Self-gravity, atomic cooling, magnetic field are all included. Stellar feedback is included through supernovae remnants, which explode immediately after a massive star formed. Momentum is injected. These models provide a reasonable description of the interstellar medium in Milky way type galaxies from a few 100 pc down to a few pc (as no adaptive mesh is being used here). Note however that the hot ionised coronal phase is not well described and consequently the galactic outflows are also not well described. These models typically lead to a reasonable star formation rate and reproduce the general trends of Larson relations. Uniform grid is used for these models.

Available simulations

standard high resolution

hydrodynamical high resolution

hydrodynamical low resolution

standard low resolution

high magnetisation low resolution

very high magnetisation low resolution

Data description

'LS' project result datafile download

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






















Experiment Result Datafile File types File size
standard high resolution LS_00041 JPEG 197.4 kB
JPEG 174.8 kB
JPEG 171.9 kB
JPEG 178.9 kB
JPEG 169.5 kB
JPEG 185.3 kB
JPEG 214.9 kB
JPEG 222.2 kB
JPEG 198.9 kB
JPEG 102.5 kB
JPEG 193.6 kB
JPEG 106.2 kB
JPEG 99.5 kB
JPEG 166.0 kB
JPEG 107.5 kB
PNG 20.3 kB
PNG 19.6 kB
PNG 23.1 kB
PNG 25.5 kB
PNG 36.3 kB
PNG 23.0 kB
LS_00049 JPEG 195.7 kB
JPEG 176.9 kB
JPEG 178.4 kB
JPEG 180.7 kB
JPEG 183.6 kB
JPEG 172.9 kB
JPEG 213.8 kB
JPEG 220.0 kB
JPEG 189.9 kB
JPEG 99.4 kB
JPEG 194.1 kB
JPEG 89.8 kB
JPEG 99.9 kB
JPEG 198.6 kB
JPEG 104.8 kB
PNG 20.4 kB
PNG 20.0 kB
PNG 23.3 kB
PNG 25.8 kB
PNG 37.0 kB
PNG 23.4 kB
hydrodynamical high resolution LS_00065 JPEG 221.2 kB
JPEG 217.1 kB
JPEG 172.4 kB
JPEG 125.3 kB
JPEG 195.1 kB
JPEG 98.1 kB
JPEG 124.1 kB
JPEG 199.9 kB
JPEG 102.4 kB
PNG 21.1 kB
PNG 19.1 kB
PNG 22.6 kB
PNG 24.9 kB
PNG 36.4 kB
hydrodynamical low resolution LS_00090 JPEG 207.3 kB
JPEG 192.6 kB
JPEG 180.7 kB
JPEG 102.7 kB
JPEG 156.0 kB
JPEG 104.0 kB
JPEG 101.0 kB
JPEG 154.3 kB
JPEG 104.1 kB
PNG 21.8 kB
PNG 19.7 kB
PNG 22.7 kB
PNG 30.9 kB
PNG 35.3 kB
LS_00150 JPEG 194.6 kB
JPEG 190.7 kB
JPEG 193.7 kB
JPEG 101.4 kB
JPEG 155.9 kB
JPEG 101.8 kB
JPEG 98.0 kB
JPEG 159.4 kB
JPEG 107.3 kB
PNG 21.7 kB
PNG 19.9 kB
PNG 23.1 kB
PNG 31.0 kB
PNG 35.9 kB
standard low resolution LS_00060 JPEG 163.6 kB
JPEG 145.6 kB
JPEG 137.6 kB
JPEG 137.1 kB
JPEG 137.8 kB
JPEG 144.9 kB
JPEG 191.1 kB
JPEG 182.1 kB
JPEG 181.5 kB
JPEG 96.9 kB
JPEG 158.6 kB
JPEG 101.4 kB
JPEG 93.2 kB
JPEG 150.1 kB
JPEG 104.4 kB
PNG 20.4 kB
PNG 19.8 kB
PNG 22.9 kB
PNG 31.9 kB
PNG 35.2 kB
PNG 22.9 kB
LS_00110 JPEG 161.3 kB
JPEG 155.7 kB
JPEG 137.9 kB
JPEG 137.6 kB
JPEG 142.7 kB
JPEG 139.8 kB
JPEG 190.7 kB
JPEG 186.9 kB
JPEG 197.2 kB
JPEG 96.7 kB
JPEG 151.6 kB
JPEG 89.4 kB
JPEG 95.0 kB
JPEG 152.4 kB
JPEG 93.2 kB
PNG 21.6 kB
PNG 19.3 kB
PNG 22.4 kB
PNG 25.2 kB
PNG 34.9 kB
PNG 23.4 kB
high magnetisation low resolution LS_00028 JPEG 173.7 kB
JPEG 179.5 kB
JPEG 191.2 kB
JPEG 98.6 kB
JPEG 144.0 kB
JPEG 90.3 kB
JPEG 99.4 kB
JPEG 149.3 kB
JPEG 92.7 kB
JPEG 162.1 kB
JPEG 135.5 kB
JPEG 133.3 kB
JPEG 138.6 kB
JPEG 137.6 kB
JPEG 137.0 kB
PNG 20.4 kB
PNG 19.6 kB
PNG 22.4 kB
PNG 31.7 kB
PNG 34.7 kB
PNG 22.9 kB
LS_00038 JPEG 174.1 kB
JPEG 181.4 kB
JPEG 179.1 kB
JPEG 95.7 kB
JPEG 151.7 kB
JPEG 90.8 kB
JPEG 100.7 kB
JPEG 151.8 kB
JPEG 93.6 kB
JPEG 167.5 kB
JPEG 142.5 kB
JPEG 132.6 kB
JPEG 136.4 kB
JPEG 135.0 kB
JPEG 130.0 kB
PNG 20.5 kB
PNG 19.8 kB
PNG 22.7 kB
PNG 25.6 kB
PNG 35.7 kB
PNG 22.8 kB
very high magnetisation low resolution LS_00020 JPEG 154.6 kB
JPEG 131.9 kB
JPEG 132.5 kB
JPEG 131.0 kB
JPEG 137.8 kB
JPEG 136.2 kB
JPEG 174.4 kB
JPEG 167.0 kB
JPEG 145.2 kB
JPEG 115.3 kB
JPEG 151.6 kB
JPEG 90.6 kB
JPEG 116.2 kB
JPEG 147.7 kB
JPEG 85.2 kB
PNG 20.3 kB
PNG 20.1 kB
PNG 22.9 kB
PNG 25.9 kB
PNG 34.9 kB
PNG 23.8 kB
LS_00030 JPEG 152.5 kB
JPEG 122.2 kB
JPEG 136.2 kB
JPEG 132.3 kB
JPEG 147.5 kB
JPEG 132.3 kB
JPEG 174.9 kB
JPEG 168.3 kB
JPEG 153.4 kB
JPEG 113.1 kB
JPEG 154.4 kB
JPEG 87.9 kB
JPEG 122.1 kB
JPEG 153.2 kB
JPEG 89.7 kB
PNG 20.4 kB
PNG 20.7 kB
PNG 22.6 kB
PNG 25.6 kB
PNG 34.8 kB
PNG 22.7 kB

This project provides images of column density, density, temperature and magnetic field. Distribution of mass, density, temperature and magnetic field are given. Clumps have been extracted using a friend-of-friend algorithm and their statistical properties (such as mass, internal velocity dispersion, size...) can be obtained. The corresponding statistics are also available. It is possible to query the clumps by specifying some requested properties. Finally the full clump data can be extracted and downloaded on demand.

 Go to top

This material is Open Data