  The two planets of the HAT-P-11 system represent fascinating dynamical
puzzles due to their significant eccentricities and orbital misalignments. In
particular, HAT-P-11 b is on a close-in orbit that tides should have
circularized well within the age of the system. Here we propose a two-step
dynamical process that can reproduce all intriguing aspects of the system. We
first invoke planet-planet scattering to generate significant eccentricities
and mutual inclinations between the planets. We then propose that this
misalignment initiated von-Zeipel-Lidov-Kozai cycles and high-eccentricity
migration that ultimately brought HAT-P-11 b to its present-day orbit. We find
that this scenario is fully consistent only when significant tidally-driven
radius inflation is accounted for during the tidal migration. We present a
suite of N-body simulations exploring each phase of evolution and show that
this scenario is consistent with all observational posteriors and the reported
age of the system.
