Paper I described the excitation of structure in the Milky Way halo due to non-local resonant excitation that occurs well inside the LMC's orbit. From the LMC's point of view, the Milky Way is in orbit about the LMC and the same dynamical coupling that raises wakes in the halo affects the LMC disk. This periodic forcing changes the angular momenta of orbits at commensurate frequencies and adds energy to the disk. In the absence of commensurabilities, the tidal forcing would be adiabatically reversible and not lead to long-term evolution (e.g. Weinberg 1994a). This is the same physics that ``heats'' stellar orbits in globular clusters (Weinberg 1994c, Murali & Weinberg 1997a, Gnedin & Ostriker 1997). In the globular cluster case, however, one is primarily concerned with the work done by the external perturbation. In a disk, a change only in the orbital angular momentum vector, with little energy transfer, can change the disk morphology.
The first subsection below illustrates the evolution based on this dynamical mechanism. The calculation is straightforward in the idealized scenario of a spheroid-dominated potential and axisymmetry and without explicit disk self gravity. It predicts significant evolution on a gigayear time scale. Including disk self gravity will lengthen the time scale but nonetheless this relatively short time scale motivates the more complete n-body treatment in §3.2.