Evolution in the Kormendy relation (μ_eff vs. r_eff in the bulges) driven by our merger experiments, compared to the observational distributions of S0s and spirals by L10. Growth vectors have been plotted, starting at the location of the original galaxy model and ending at the μ_eff-r_eff values of the remnants. The growth vectors corresponding to the merger models with dense spheroidal satellites by Aguerri et al. (2001) are represented. In both cases, the evolution induced by the mergers in the plane is negligible. The scalings as we detailed in Sect. 4 have been assumed for all plots, but note that the models can be scaled in mass and size. The location of Coma cluster ellipticals from Khosroshahi et al. (2000) is marked with a solid line. Consult the legend for the observational data and the models in the figure.