  Remnant planetesimals might have played an important role in reducing the
orbital eccentricities of the terrestrial planets after their formation via
giant impacts. However, the population and the size distribution of remnant
planetesimals during and after the giant impact stage are unknown, because
simulations of planetary accretion in the runaway growth and giant impact
stages have been conducted independently. Here we report results of direct
N-body simulations of the formation of terrestrial planets beginning with a
compact planetesimal disk. The initial planetesimal disk has a total mass and
angular momentum as observed for the terrestrial planets, and we vary the width
(0.3 and 0.5AU) and the number of planetesimals (1000-5000). This initial
configuration generally gives rise to three final planets of similar size, and
sometimes a fourth small planet forms near the location of Mars. Since a
sufficient number of planetesimals remains, even after the giant impact phase,
the final orbital eccentricities are as small as those of the Earth and Venus.
