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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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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
Ugo LEBREUILLY  

DISKS_POPULATIONS

  • Summary
  • Available simulations
    • NIMHD
    • IMHD
    • HYDRO

Summary

This project treats the evolution of massive star forming clumps under self-gravity, radiative transfer and non-ideal MHD turbulence. Here we apply this treatment to study the disk formation specifically (see Lebreuilly et al., 2021 for reference paper). The spherical cloud has an initial mass of about 1000 Msun. A turbulent field is initially set within the cloud. The adaptive mesh refinement scheme is employed to resolve scales up to about ~1 AU. When a density of about 10^{13} cm^-3 is reached, a sink particle is introduced. Radiative stellar feedback is treated here and the turbulence is free to decay.

Available simulations

NIMHD

IMHD

HYDRO

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This material is Open Data