Abstract

Accretion disks are the birthplace of planets. A young planet interacts with its surrounding disk, launching spiral density waves that lead to the formation of rings and gaps observable with ALMA . The disk, in turn, exerts a torque on the planet, causing it to migrate through the disk. The role of radiative processes in these mechanisms has recently become more important, as our understanding of the thermodynamics improves and the complexity of models increases. I will present how cooling and specifically in-plane radiative diffusion affect planet-driven gap opening, and show that models with more realistic thermodynamics can produce higher-quality synthetic observations of ALMA disks with substructures. I will then show how radiation transport can impact the dynamical corotation torque, effectively accelerating or decelerating the planet’s orbital evolution depending on context.