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Ionization impact on molecular clouds and star formation Numerical simulations and observations

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Figure

Figure 3 – Carte de densité de colonne de la nébuleuse de la Rosette observée par Herschel.
Figure 1.1: Schmidt-Kennicutt law from Kennicutt (1998). The power law fit gives an exponent of 1.4 ± 0.15.
Figure 2.3: Radiation driven implosion from Bisbas et al. (2009) with the same parameters as Lefloch and Lazareff (1994) for the cloud.
Figure 2.4: Formation of pillars in turbulent simulations of Gritschneder et al. (2009).
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