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Fig. 7


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H2 formation rate as a function of the uv field intensity (in units of the Habing interstellar field) for various proton number density. Data adapted from Fig. 6 of Bron et al. (2014) are shown as the blue (104 cm−3) and purple (106 cm−3) solid lines, while black lines correspond to our analytic fit for four different number densities (104, 106, 107, 108 cm−3).

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