Left: the total torque profile of our standard disk in units of Γ₀ is shown in red. The dashed blue curve shows the true torque profile for a 10  m_⊕ planet near an opacity transition, calculated using the equations in Paardekooper et al. (2011). Right: decrease in the corotation torque Γ_C as a function of planetary eccentricity e. We assume that the damping (0 < D < 1) of the corotation torque as a function of eccentricity is the same for isothermal and fully radiative disc. Then, we derived D from Fig. 2 of Bitsch & Kley (2010) by taking the difference between their fully radiative and isothermal case, and normalizing to 1 the “e = 0 case”.