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Planetary embryos uniformly distributed in the inner region of the The first simulations of terrestrial planet formation (Chambers and Wetherill, 1998) included a set of In general, simulations of the dynamical re-shaping of the Asteroidīelt are made in conjunction with the formation of the inner Jupiter and Saturn, which have a major influence on the dynamicalĮvolution of the Asteroid Belt and its final orbital structure. Also, we constrain the primordial eccentricities of Nearly unchanged with a slight preference for depletion at low inclination this leads to the conclusion that the inclination distribution at the end of the Grand Tack is a bit over-excited. Similar to that currently observed, and the semimajor axis distribution does the same. Our results show that the eccentricityĭistribution obtained in the Grand Tack model evolves towards one very The model continues for an additional 4.1 Gy after Before the instability, the terrestrial planets were modeled onĭynamically cold orbits with Jupiter and Saturn locked in a 3:2 mean Including an instability of the Giant Planets approximately 400 My Of the gas nebula phase when planets emerge from the dispersing gasĭisk), throughout the subsequent evolution of the Solar System Of the Asteroid Belt from the end of the Grand Tack model (at the end Here, we evaluate the evolution of the orbital properties The Grand Tack model is in good agreement with the one observed, theĮccentricity distribution is skewed towards values larger than thoseįound today. However, while the inclination distribution produced in Reconciling the small mass of Mars with the properties of the Asteroidīelt, including the mass depletion, radial mixing and orbitalĮxcitation. Grand Tack model presents a possible solution to the conundrum of
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Is strongly linked to the process of terrestrial planet formation. Models of theĮvolution of the Asteroid Belt show that the origin of its structure
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Solar Nebula expectations and has an excited orbital distribution, withĮccentricities and inclinations covering the entire range of valuesĪllowed by the constraints of dynamical stability. The Asteroid Belt is characterized by the radial mixing of bodies withĭifferent physical properties, a very low mass compared to Minimum Mass