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The asteroid belt is characterized by an extreme low total mass of materialon dynamically excited orbits. The Nice Model explains many peculiar qualitiesof the solar system, including the belt's excited state, by invoking an orbitalinstability between the outer planets. However, previous studies of the NiceModel's effect on the belt's structure struggle to reproduce the innermostasteroids' orbital inclination distribution. Here, we show how the final phaseof giant planet migration sculpts the asteroid belt, in particular itsinclination distribution. As interactions with leftover planetesimals causeSaturn to move away from Jupiter, its rate of orbital precession slows as thetwo planets' mutual interactions weaken. When the planets approach their modernseparation, where Jupiter completes just short of five orbits for every two ofSaturn's, Jupiter's eccentric forcing on Saturn strengthens. We use numericalsimulations to show that the absence of asteroids with orbits that precessbetween 24-28 arcsec/yr is related to the inclination problem. As Saturn'sprecession speeds back up, high inclination asteroids are excited on to planetcrossing orbits and removed from the inner main belt. Through this process, theasteroid belt's orbital structure is reshaped, leading to markedly improvedsimulation outcomes.

A record of the final phase of giant planet migration fossilized in the asteroid belt's orbital structure