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Fig. 3
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Dust densities for the XEUV-irradiated primordial disk in (R, z) for a ‘fixed’ dust-to-gas ratio throughout the disk. Enough material of all grain sizes is present at the base of the XEUV-driven outflow, resulting in high dust densities in the wind. Due to the model setup, the disk-wind interface is clearly discernible.
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