Fig. 6
Spectral energy distribution resulting from the radiative transfer modelling, assuming grain size distribution after 1 Myr of evolution when two planets interact with the disk, and assuming different values for the disk viscosity αturb and fragmentation velocity of particles vf. The disk data are for SR 21 and are taken from Brown et al. (2007); Follette et al. (2013) and PACS (DIGIT PI: N. Evans).
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