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Subsequent to the Moon's formation, late accretion to the terrestrial planetsmodified their silicate crusts and mantles. We combine dynamical N-body andMonte Carlo simulations to determine impact probabilities, impact velocities,and expected mass augmentation onto the terrestrial planets from three sources:planetesimals left over from primary accretion, asteroids from the E-belt, andcomets arriving from the outer Solar System. We present estimates of the amountof cometary material striking the terrestrial planets in an early episode ofplanetesimal-driven giant planet migration (Mojzsis et al., 2019). The Moon andMars suffer proportionally higher cometary accretion than Venus and Earth. Thebackground mass addition from small leftover planetesimals to Earth and Mars isfar less than independent estimates based on their mantle abundances ofhighly-siderophile elements. This supports the theory that both planets werestruck by single large bodies that delivered most of their mass augmentationsince primary accretion. We present fits to the impact chronologies valid from4500 Ma to ca. 3700 Ma. The lunar timeline thus obtained is at odds with boththe calibrated Neukum (Neukum et al., 2001) and Werner (Werner et al., 2014;Werner, 2019) chronologies. For Mars, the match with its calibrated Wernerchronology is no better; by increasing the mass of the E-belt by a factor offour the dynamical lunar and martian chronologies are in line with that ofWerner (2019) and match constraints from the current population of Hungariaasteroids. Yet, neither of our dynamical timelines fit well with that ofNeukum. The dynamical lunar and martian chronologies are also different fromeach other. Consequently, the usual extrapolation of such chronologies from oneplanetary body to the other is technically inappropriate.

Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga