I present an overview of the components of the asteroseismic surface effect, which can be divided into a modal part and a structural part. I discuss best practices in evaluating the structural part, which is entirely due to differences in mean stratification between the seismically observed star and our model of it. Assuming this part is due to the 3D nature of surface convection, the structural part of the surface effect can be found as the frequency differences between an averaged 3D convection simulation, and a 1D (MLT) model mathched to that simulation.