The figure shows an example of cumulative core scouring in our model. The y-axis shows the surface mass density of the remnant bulge divided by the stellar mass of the remnant, while the x-axis shows radial distance. Prior to the initial gas-rich merger, the primary progenitor is set to have a Hernquist profile (λ₀ = 1.0). The new, postmerger inner density slope λ_p is then set using Equation (9). A subsequent gas-poor merger delivers a secondary black hole that forms a binary with the primary, scouring out a core (λ₁). Each successive dry merger results in shallower profiles each time (λ₂ and λ₃), culminating after the final merger in a profile with inner logarithmic slope λ_c. The shaded region represents the stellar mass deficit.