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Interstellar Molecular clouds and star formation

The density structure of the interstellar medium is highly inhomogeneous and fractal.
The regions with higher gas density are more prone to self-gravitational collapse, which eventually lead to star formation.

Here we visualize the density structure around a molecular cloud as obtained by hydrodynamic simulations (the SILCC project). The simulation includes important heating and cooling gas processes (photoelectric heating radiative cooling), chemistry (H, H2, C, CO, etc.), gravity, and energy injection by stellar radiation and supernova.

The visualization was made possible thanks to 
pycharm
plotly
github

Walch et al. (2015)

Seifried et al.  (2017)

Siefried et al. (2020)

Bialy et al. (in prep)

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