  Mass-independent isotopic anomalies of carbonaceous and non-carbonaceous
meteorites show a clear dichotomy suggesting an efficient separation of the
inner and outer solar system. Observations show that ring-like structures in
the distribution of mm-sized pebbles in protoplanetary disks are common. These
structures are often associated with drifting pebbles being trapped by local
pressure maxima in the gas disk. Similar structures may also have existed in
the sun's natal disk, which could naturally explain the meteorite/planetary
isotopic dichotomy. Here, we test the effects of a strong pressure bump in the
outer disk (e.g. $\sim$5~au) on the formation of the inner solar system. We
model dust coagulation and evolution, planetesimal formation, as well as
embryo's growth via planetesimal and pebble accretion. Our results show that
terrestrial embryos formed via planetesimal accretion rather than pebble
accretion. In our model, the radial drift of pebbles foster planetesimal
formation. However, once a pressure bump forms, pebbles in the inner disk are
lost via drift before they can be efficiently accreted by embryos growing at
$\gtrapprox$1~au. Embryos inside $\sim$0.5-1.0au grow relatively faster and can
accrete pebbles more efficiently. However, these same embryos grow to larger
masses so they should migrate inwards substantially, which is inconsistent with
the current solar system. Therefore, terrestrial planets most likely accreted
from giant impacts of Moon to roughly Mars-mass planetary embryos formed around
$\gtrapprox$1.0~au. Finally, our simulations produce a steep radial mass
distribution of planetesimals in the terrestrial region which is qualitatively
aligned with formation models suggesting that the asteroid belt was born
low-mass.
