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Isotopic anomalies provide a means of probing the materials responsible forthe formation of terrestrial planets. By analyzing new iron isotopic anomalydata from Martian meteorites and drawing insights from published data for O,Ca, Ti, Cr, Fe, Ni, Sr, Zr, Mo, Ru, and Si, we scrutinize potential changes inthe isotopic composition of the material accreted by Mars and Earth duringtheir formation.  A Principal Component Analysis of isotopic anomalies in meteorites identifiesthree main clusters (forming the three parts of the isotopic trichotomy): CI,CC=CM+CO+CV+CR, and NC=EH+EL+H+L+LL.  Our results suggest that Earth is primarily an isotopic mixture of ~92% E, 6% CI, and <2% COCV and O. Mars, on the other hand, appears to be a mixture of~65% E, 33% O, and <2% CI and COCV. We establish that Earth's CI contributionsubstantially increased during the latter half of its accretion. Mars beganaccreting a mix of O and E but predominantly accreted E later.  Mars' changing isotopic makeup during accretion can be explained if itunderwent gas-driven type I migration from its origin near the O - E boundaryto a location well within the E region during the first few million years ofsolar system history. Earth's later increased CI contribution may be attributedto the stochastic impact of an interloper carbonaceous embryo that moved insidethe inner solar system region while nebular gas was still present, andsubsequently participated in the stage of chaotic growth.  The recent findings of Si isotopic anomalies in enstatite chondrites whencompared to terrestrial rocks likely stems from insufficient correction forhigh-temperature equilibrium isotopic fractionation. With appropriateadjustments for this influence, both the silicate Earth and enstatitechondrites exhibit comparable Si isotopic anomalies, reaffirming a genetic linkbetween them.

Bayesian Inference on the Isotopic Building Blocks of Mars and Earth