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The Asteroid Belt is characterized by the radial mixing of bodies withdifferent physical properties, a very low mass compared to Minimum Mass SolarNebula expectations and has an excited orbital distribution. Models of theevolution of the Asteroid Belt show that the origin of its structure isstrongly linked to the process of terrestrial planet formation. The Grand Tackmodel presents a possible solution to the conundrum of reconciling the smallmass of Mars with the properties of the Asteroid Belt, including the massdepletion, radial mixing and orbital excitation. However, while the inclinationdistribution produced in the Grand Tack model is in good agreement with the oneobserved, the eccentricity distribution is skewed towards values larger thanthose found today. Here, we evaluate the evolution of the orbital properties ofthe Asteroid Belt from the end of the Grand Tack model (at the end of the gasnebula phase when planets emerge from the dispersing gas disk), throughout thesubsequent evolution of the Solar System including an instability of the GiantPlanets approximately 400 My later. Before the instability, the terrestrialplanets were modeled on dynamically cold orbits with Jupiter and Saturn lockedin a 3:2 mean motion resonance. The model continues for an additional 4.1 Gyafter the giant planet instability. Our results show that the eccentricitydistribution obtained in the Grand Tack model evolves towards one very similarto that currently observed, and the semimajor axis distribution does the same.The inclination distribution remains nearly unchanged with a slight preferencefor depletion at low inclination; this leads to the conclusion that theinclination distribution at the end of the Grand Tack is a bit over-excited.

Is the Grand Tack model compatible with the orbital distribution of main belt asteroids?