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The diverse isotopic anomalies of meteorites demonstrate that theprotoplanetary disk was composed of components from different stellar sources,which mixed in the disk and formed the planetary bodies. However, the origin ofthe accretion materials of different planetary bodies and the cosmochemicalrelationship between these bodies remain ambiguous. The noncarbonaceous (NC)planetary bodies originate from the inner solar system and have isotopiccompositions distinct from those of the carbonaceous (CC) bodies. We combinedCa, Ti, Cr, Fe, Ni, Mo, and Ru isotopic anomalies to develop a quantitativetwo-endmember mixing model of the NC bodies. Correlations of the isotopicanomalies of different elements with different cosmochemical behaviorsoriginate from the mixing of two common endmembers. Using this mixing model, wecalculated the isotopic anomalies of NC bodies for all the considered isotopes,including the isotopic anomalies that are difficult to measure or have beenaltered by spallation processes. The mixing proportion between the twoendmembers in each NC body has been calculated as a cosmochemical parameter,which represents the compositional relationship of the accretion materialsbetween the NC bodies. Using the calculated mixing proportions, the feedingzones of the NC bodies could be estimated. The estimated feeding zones of NCbodies indicate a large population of interlopers in the main asteroid belt andan indigenous origin of Vesta. The feeding zones estimated in different planetformation scenarios indicate that the orbits of Jupiter and Saturn duringformation of terrestrial planets were likely to be more circular than theircurrent ones.

Accretion regions of meteorite parent bodies inferred from a two-endmember isotopic mixing model