  Stars are commonly formed in binary systems, which provide a natural
laboratory for studying planet formation in extreme conditions. In our first
paper (Paper I) of a series Xie et al. (2011), we have shown that the
intermediate stage - from planetesimals to planetary embryos/cores - of planet
formation can proceed even in highly inclined binaries. Following Paper I, here
we numerically study the late stage of terrestrial planet formation, i.e., from
embryos to full planets, in binary systems of various orbital configurations.
We identify an orbital alignment or anti-alignment effect; namely, although an
inclined binary generally misaligns the planetary orbits with respect to the
spin axis of the primary host star (i.e., causing large obliquity), it could
align or anti-align the planetary orbits with respect to the binary orbit. Such
an orbital (anti-)alignment effect is caused by the combination of orbital
differential precession and self-damping, and it is mostly significant in cases
of intermediate binary separations, i.e., a_B~40-200 AU for terrestrial planet
formation around 1 AU from the primary stars. In such intermediate separation
binaries, somewhat contrary to intuition, the binary companion can aid planet
growth by having increased the rate of collisions, forming significantly more
massive but fewer planets. In the other two ends, the companion is ether too
close thus plays a violently disruptive role or too wide to have significant
effect on planet formation. Future observations, which can discover more
planet-bearing binary star systems and constrain their masses and 3-D orbital
motions will test our numerical findings.
