Azimuthally averaged eccentricities in the “wide” (dotted black) and “tight” (solid black) version of model #8 (m_pl = 8M_J, m_∗ = 1   M_⊙) and the atmospheric temperature (red). It is apparent that even though the eccentricity maximum is smaller in the “wide” system, the disk is more eccentric on average than in the “tight” model. At the same time the planet signal becomes stronger in the “tight” (see Fig. 8f) than in the “wide” (see Fig. 8e) model, because the disk atmosphere is considerably hotter at 0.5 AU than 2 AU, where the disk is dynamically perturbed by the planet.