There are no simple formulae describing the warp amplitudes in general because of the complexity of the interaction. Qualitative guidelines are as follows. Within the range of scenarios explored here, the most important condition is the coincidence of wake pattern speed and the disk bending-mode frequency. Exploration suggests the 2:1 resonance between the satellite and orbital azimuthal frequencies and the ILR-like resonance are most important. A secondary consideration is the location and amplitude of the wake itself which depends on the halo profile and the existence of low-order resonances in the vicinity of the disk. These two features are not independent. However, if one could fix the orbital frequencies of halo stars, the wake amplitude would be proportional to the halo density and if one could fix the density, the wake location would scale with the orbital frequencies. The halos considered here are chosen to have flat rotation curves between the outer disk and satellite pericenter. Because the wake is dominated by the 2:1 resonance, the wake peaks at roughly half the pericenter distance. Therefore, increasing the mass of the halo will tend to increase the wake amplitude but can decrease the disk warp if the frequency match with the global disk modes is less favorable.
Because of this complicated interplay and sensitivity to the actual disk and halo profiles, I will illustrate the range of possibilities with some examples rather than give an exhaustive set of models.