  We calculate herein the late stages of terrestrial planet accumulation around
a solar type star that has a binary companion with semimajor axis larger than
the terrestrial planet region. We perform more than one hundred simulations to
survey binary parameter space and to account for sensitive dependence on
initial conditions in these dynamical systems. As expected, sufficiently wide
binaries leave the planet formation process largely unaffected. As a rough
approximation, binary stars with periastron $q_B > 10$ AU have minimal effect
on terrestrial planet formation within $\sim 2$ AU of the primary, whereas
binary stars with $q_B \la$ 5 AU restrict terrestrial planet formation to
within $\sim$ 1 AU of the primary star. Given the observed distribution of
binary orbital elements for solar type primaries, we estimate that about 40 --
50 percent of the binary population is wide enough to allow terrestrial planet
formation to take place unimpeded. The large number of simulations allows for
us to determine the distribution of results -- the distribution of plausible
terrestrial planet systems -- for effectively equivalent starting conditions.
We present (rough) distributions for the number of planets, their masses, and
their orbital elements.
