Perturbed surface density at t = 150 orbits at the planet location (top panels) and at t = 500 (bottom panels) orbits. From left to right: simulation sets HD_iso, HD_βc with β_c = 1, HD_rad, and HD_βc with β_c = 100, HD_adia. We observe multiple rings formation that depend on the EoS. Rings are persistent on longer integration times. For the radiative case, we report the last snapshot, i.e. the one at 150 orbits in the bottom panel.