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Fig. 5


Overview of one of the DALI models showing the disk structure, abundance structure and emitting regions for the Q(6) 0110 and R(7) 0001 lines. The model shown has a gas-to-dust ratio, g/dgas = 1000 and a constant CO2 abundance of 10-7 with respect to H. The panels show: a) gas density structure; b) abundance structure used models: xin and xout are the CO2 abundances in the inner and outer region respectively, the grey region is part of the outer region and denotes the region around the CO2 iceline where planetesimals are assumed to vaporize. The abundance in this region is varied in the models in Sect. 4.2; c) line contribution function of the Q(6) 0110 line at 15 μm, the contours show the areas in which 25% and 75% of the total flux is emitted; d) contribution function for the R(7) 0001 line at 4.3 μm. Panels c) and d) have the τ = 1 surface of dust (blue) and line (red) and the n = ncrit surface (black) overplotted for the relevant line.

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