  Recent improvements to GPU hardware and the symplectic N-body code GENGA
allow for unprecedented resolution in simulations of planet formation. In this
paper, we report results from high-resolution N-body simulations of terrestrial
planet formation that are mostly direct continuation of our previous 10 Myr
simulations (Woo et al. 2021a) until 150 Myr. By assuming that Jupiter and
Saturn have always maintained their current eccentric orbits (EJS), we are able
to achieve a reasonably good match to the current inner solar system
architecture. However, due to the strong radial mixing that occurs in the EJS
scenario, it has difficulties in explaining the known isotopic differences
between bodies in the inner solar system, most notably between Earth and Mars.
On the other hand, assuming initially circular orbits for Jupiter and Saturn
(CJS) can reproduce the observed low degree of radial mixing in the inner solar
system, while failing to reproduce the current architecture of the inner solar
system. These outcomes suggest a possible paradox between dynamical structure
and cosmochemical data for the terrestrial planets within the classical
formation scenario.
