Abstract
Protoplanets interact with their natal disks and can generate prominent gas and dust substructures such as gaps and rings. However, it remains unclear how these planet-induced substructures modify the disk temperature and how the resulting temperature changes subsequently affect the substructures. To address this, we perform iterative multi-fluid hydrodynamical and Monte Carlo radiative transfer simulations of planet–disk interactions. We find that the temperature in a structured disk deviates significantly from that of a smooth disk due to giant planet formation. In particular, a deep gap carved by a giant planet can increase the local disk temperature by several tens of kelvin. Such temperature variations can shift the locations of volatile ice lines, potentially leading to the formation of multiple dust rings, as confirmed by our dust evolution simulations. These findings may explain the lack of a simple correlation between dust ring positions and ice line locations inferred from assumed smooth-disk temperature profiles in recent ALMA surveys.
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