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The discovery of Jupiter-mass planets in close orbits about their parentstars has challenged models of planet formation. Recent observations have shownthat a number of these planets have highly inclined, sometimes retrogradeorbits about their parent stars, prompting much speculation as to their origin.It is known that migration alone cannot account for the observed population ofthese misaligned hot Jupiters, which suggests that dynamical processes afterthe gas disc dissipates play a substantial role in yielding the observedinclination and eccentricity distributions. One particularly promisingcandidate is planet-planet scattering, which is not very well understood in thenon-linear regime of tides. Through three-dimensional hydrodynamicalsimulations of multi-orbit encounters, we show that planets that are scatteredinto an orbit about their parent stars with closest approach distance beingless than approximately three times the tidal radius are either destroyed orcompletely ejected from the system. We find that as few as 5 and as many as 18of the currently known hot Jupiters have a maximum initial apastron forscattering that lies well within the ice line, implying that these planets musthave migrated either before or after the scattering event that brought them totheir current positions. If stellar tides are unimportant $(Q_\ast \gtrsim10^7)$, disk migration is required to explain the existence of the hot Jupiterspresent in these systems. Additionally, we find that the disruption and/orejection of Jupiter-mass planets deposits a Sun's worth of angular momentumonto the host star. For systems in which planet-planet scattering is common, wepredict that planetary hosts have up to a 35% chance of possessing an obliquityrelative to the invariable plane of greater than 90 degrees.

Consequences of the Ejection and Disruption of Giant Planets