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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

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Resolving protoplanetary disks in massive protostellar clumps

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Extreme Horizons

Resolving galactic disks in their cosmic environment

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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=$428.9 \; \textrm{Myr}$)

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This material is Open Data