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Fig. 2

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Physical structure of the multi-grain models incorporating a full dust distribution. The quantity Tg is the gas temperature, nH is the gas number density, G is the local stellar and interstellar field in the case of the HUV models (see Appendix A), ζis the dust togas mass ratio, Ta (Eq. (1)) is the area-weighted dust temperature, and na is the area-weighted grain number density. The quantity AV is the visualextinction counted from disk surface toward the disk midplane.

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