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N-body numerical simulations code for the orbital motion ofasteroids/planetesimals within the asteroid belt under the gravitationalinfluence of the sun and the accreting planets has been developed. The aim isto make qualitative, and to an extent a semi-quantitative argument, regardingthe possible extent of radial mixing and homogenization of planetesimalreservoirs of the two observed distinct spectral types , viz., the S-type andC-type, across the heliocentric distances due to their dynamical orbitalevolution, thereby, eventually leading to the possible accretion of asteroidshaving chemically diverse constituents. The spectral S-type and C-typeasteroids are broadly considered as the parent bodies of the two observed majormeteoritic dichotomy classes, namely, the non-carbonaceous (NC) andcarbonaceous (CC) meteorites, respectively. The present analysis is performedto understand the evolution of the observed dichotomy and its implications dueto the nebula and early planetary processes during the initial 10 Myrs (Millionyears). The homogenization across the two classes is studied in context to theaccretion timescales of the planetesimals with respect to the half-life of thepotent planetary heat source, 26Al. The accretion over a timescale of ~1.5 Myr.possibly resulted in the planetary-scale differentiation of planetesimals toproduce CC and NC achondrites and iron meteorite parent bodies, whereas, theprolonged accretion over a timescale of 2-5 Myrs. resulted in the formation ofCC and NC chondrites. Our simulation results indicate a significant role of theinitial eccentricities and the masses of the accreting giant planets,specifically, Jupiter and Saturn, in triggering the eccentricity churning ofthe planetesimals across the radial distances

Dynamical orbital evolution of asteroids and planetesimals across  distinct chemical reservoirs due to accretion growth of planets in the early  solar system