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. 2021 Feb 17;7(8):eabc0444. doi: 10.1126/sciadv.abc0444

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Copyright © 2021 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works. Distributed under a Creative Commons Attribution NonCommercial License 4.0 (CC BY-NC).

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Fig. 4 — (A) Numerical growth tracks of protoplanets growing by pebble accretion and planetesimal accretion, starting at r₀ = 1.6 AU. The parameters of the growth track were chosen with Venus and Mars as end-members. Earth obtains a final mass of 0.6 M_E, which we augment by creating Theia slightly later to reach a final mass of 0.4 M_E. (B) Masses of the four planets as a function of time. We show here also the contribution from planetesimal accretion in the birth belt. (C) The fraction of mass accreted from outer Solar System material, as a function of the time when the drifting pebbles change to CI composition. We find agreement with the estimated CI contribution of 42% to Earth and 36% to Mars (36) for a transition time from ureilite composition to CI composition in the range 3.5 Ma to 4.0 Ma.