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Rings and gaps are ubiquitous in protoplanetary disks. Larger dust grainswill concentrate in gaseous rings more compactly due to stronger aerodynamicdrag. However, the effects of dust concentration on the ring's thermalstructure have not been explored. Using MCRT simulations, we self-consistentlyconstruct ring models by iterating the ring's thermal structure, hydrostaticequilibrium, and dust concentration. We set up rings with two dust populationshaving different settling and radial concentration due to their differentsizes. We find two mechanisms that can lead to temperature dips around thering. When the disk is optically thick, the temperature drops outside the ring,which is the shadowing effect found in previous works adopting a single-dustpopulation in the disk. When the disk is optically thin, a second mechanism dueto excess cooling of big grains is found. Big grains cool more efficiently,which leads to a moderate temperature dip within the ring where big dustresides. This dip is close to the center of the ring. Such temperature dipwithin the ring can lead to particle pile-up outside the ring and feedback tothe dust distribution and thermal structure. We couple the MCRT calculationswith a 1D dust evolution model and show that the ring evolves to a differentshape and may even separate to several rings. Overall, dust concentrationwithin rings has moderate effects on the disk's thermal structure, andself-consistent model is crucial not only for protoplanetary disk observationsbut also for planetesimal and planet formation studies.

Self-consistent ring model in protoplanetary disks: temperature dips and substructure formation