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Galactica

Turbulent flow in the interstellar medium

Galactic disk

Gas fragmentation in the ISM

Cosmological structures

Mare Nostrum simulation

Cosmological structures

Solar magnetic field

Solar magnetic field

Extreme Horizons

Extreme Horizons

Resolving galactic disks in their cosmic environment

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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

This model has an initial resolution of about 2 pc and a finest grid after zooming of about 400 AU.

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This material is Open Data