Estimates of the perturbed surface density expected after 100 planetary orbits for the models featured in Fig. 2 (using ∂F_dep/∂R from Fig. 2, Eq. (20), and the method in Cordwell & Rafikov 2024). The adiabatic and isothermal models show a double-trough gap structure, while radiative models show a single, deep gap. An apparent third dip in the adiabatic model at R = R_p is related to the perturbations driven by buoyancy modes near the edge of the planet’s horseshoe region.