  The final stage in the formation of terrestrial planets consists of the
accumulation of ~1000-km ``planetary embryos'' and a swarm of billions of 1-10
km ``planetesimals.'' During this process, water-rich material is accreted by
the terrestrial planets via impacts of water-rich bodies from beyond roughly
2.5 AU. We present results from five high-resolution dynamical simulations.
These start from 1000-2000 embryos and planetesimals, roughly 5-10 times more
particles than in previous simulations.
  Each simulation formed 2-4 terrestrial planets with masses between 0.4 and
2.6 Earth masses. The eccentricities of most planets were ~0.05, lower than in
previous simulations, but still higher than for Venus, Earth and Mars. Each
planet accreted at least the Earth's current water budget.
  We demonstrate several new aspects of the accretion process: 1) The feeding
zones of terrestrial planets change in time, widening and moving outward. Even
in the presence of Jupiter, water-rich material from beyond 2.5 AU is not
accreted for several millions of years. 2) Even in the absence of secular
resonances, the asteroid belt is cleared of >99% of its original mass by
self-scattering of bodies into resonances with Jupiter. 3) If planetary embryos
form relatively slowly, following the models of Kokubo & Ida, then the
formation of embryos in the asteroid belt may have been stunted by the presence
of Jupiter. 4) Self-interacting planetesimals feel dynamical friction from
other small bodies, which has important effects on the eccentricity evolution
and outcome of a simulation.
