  Core-accretion planet formation begins in protoplanetary disks with the
growth of small, ISM dust grains into larger particles. The progress of grain
growth, which can be quantified using 10 micron silicate spectroscopy, has
broad implications for the final products of planet formation. Previous studies
have attempted to correlate stellar and disk properties with the 10 micron
silicate feature in an effort to determine which stars are efficient at grain
growth. Thus far there does not appear to be a dominant correlated parameter.
In this paper, we use spatially resolved adaptive optics spectroscopy of 9 T
Tauri binaries as tight as 0.25" to determine if basic properties shared
between binary stars, such as age, composition, and formation history, have an
effect on dust grain evolution. We find with 90-95% confidence that the
silicate feature equivalent widths of binaries are more similar than those of
randomly paired single stars, implying that shared properties do play an
important role in dust grain evolution. At lower statistical significance, we
find with 82% confidence that the secondary has a more prominent silicate
emission feature (i.e., smaller grains) than the primary. If confirmed by
larger surveys, this would imply that spectral type and/or binarity are
important factors in dust grain evolution.
