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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

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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
Patrick HENNEBELLE  

FRIG

  • Summary
  • Available simulations
    • FRIGG

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 and to zoom onto dense cores. It is described in Hennebelle 2018, A&A, 611, 24. 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 immediatly 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 hundreds of AU (as intensive 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 population of dense cores.

Available simulations

FRIGG

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This material is Open Data