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The solar system's dynamical state can be explained by an orbital instabilityamong the giant planets. A recent model has proposed that the giant planetinstability happened during terrestrial planet formation. This scenario hasbeen shown to match the inner solar system by stunting Mars' growth andpreventing planet formation in the asteroid belt. Here we present a largesample of new simulations of the "Early Instability" scenario. We use an N-bodyintegration scheme that accounts for collisional fragmentation, and alsoperform a large set of control simulations that do not include an early giantplanet instability. Since the total particle number decreases slower whencollisional fragmentation is accounted for, the growing planets' orbits aredamped more strongly via dynamical friction and encounters with small bodiesthat dissipate angular momentum (eg: hit-and-run impacts). Compared withsimulations without collisional fragmentation, our fully evolved systemsprovide better matches to the solar system's terrestrial planets in terms oftheir compact mass distribution and dynamically cold orbits. Collisionalprocesses also tend to lengthen the dynamical accretion timescales of Earthanalogs, and shorten those of Mars analogs. This yields systems with relativegrowth timescales more consistent with those inferred from isotopic dating.Accounting for fragmentation is thus supremely important for any successfulevolutionary model of the inner solar system.

The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation