Abundance of CO₂ as function of radii for models with different destruction rates of CO₂. These modeluse α = 10⁻³ and u_f = 0 m s⁻¹ (left) and u_f = 3 m s⁻¹ (right). Abundance profiles after 1 Myr of evolution are shown. At this point the disk has reached a semi steady state. A destruction rate of at least 10⁻¹¹ s⁻¹ is needed to keep the averaged CO₂ abundance below the observational limit. The iceline is further out for models with higher destruction rates as the destruction of gas-phase CO₂ lowers the total abundance of CO₂ within 10 AU where CO₂ can sublimate.