•  Home
  •  Topics 
    •  Solar Magnetohydrodynamics
    •  Star-planet interactions
    •  Star formation
    •  Galaxy formation
    •  Cosmology
  •  About
  •  Log in
Galactica

Turbulent flow in the interstellar medium

Galactic disk

Gas fragmentation in the ISM

HD189733 wind

Wind of HD 189733

Unveiling the magnetic link between stars and planets

Synthetic disk populations

Synthetic disk populations

Resolving protoplanetary disks in massive protostellar clumps

Solar magnetic field

Solar magnetic field

Extreme Horizons

Extreme Horizons

Resolving galactic disks in their cosmic environment

Previous Next
  1. Home
  2. Star formation
  3. M51SIM
  4. Isolated

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
Robin TRESS  

Isolated

  • Summary
  • Snapshots
    • t=$217.1 \; \textrm{Myr}$
    • t=$428.9 \; \textrm{Myr}$

Summary

In this case the disc galaxy is evolved in isolation and hence the morphology remains flocculent throughout the simulation time.

Simulated using Arepo

Snapshots

Snap_ISO_1109 (t=$217.1 \; \textrm{Myr}$)

Snap_ISO_2192 (t=$428.9 \; \textrm{Myr}$)

 Go to top

This material is Open Data