  The formation and subsequent migration of gas giants could significantly
affect the material mixing in the Solar System. In this study, we use N-body
simulations to investigate how much water is transported into the region of the
terrestrial planet formation during the growth and migration phases of Jupiter
in the Grand Tack model. We found that Jupiter's growth was accompanied by
significant mass transport, and that a substantial amount of water (about 10
times Earth's ocean mass for the initial planetesimal distribution based on the
minimum-mass solar nebula) was transported into the terrestrial planet region.
The total amount delivered increased further during Jupiter's migration phase
(totaling about 10-40 times Earth's ocean mass), which was less dependent on
simulation parameters. In addition, at these stages, terrestrial planets were
not fully grown. Therefore, water supplied during these early stages could
interact with metallic iron during the core formation of protoplanets and/or
growing Earth. Since hydrogen in water molecules can dissolve into their cores,
this could explain the density deficit observed in the current Earth core.
Notably, Jupiter could play an important role as a ''barrier'' in explaining
the dichotomy of the isotopic compositions between noncarbonaceous (NC) and
carbonaceous (CC) meteorites. This study's results show that Jupiter's growth
necessitates some mixing of NC and CC materials.
