  Accretion is one of the defining characteristics of classical T Tauri stars,
fueled by the presence of a circumstellar disk comprised of dust and gas.
Accretion produces a UV and optical excess, while re-radiated emission at the
inner edge of the dust component of the disk produces a near-infrared (NIR)
excess. The interplay between stars and their disks helps regulate
protoplanetary disk evolution and dispersal, which is key to a full
understanding of planet formation. To investigate the relations between NIR
excess and optical excess in both single and binary stars, we used an archival
sample of spectroscopically characterized members of the Taurus star-forming
region ($\tau \sim$ 1-2 Myr) with measured luminosities, spectral types, and
optical veiling. We combined the archival sample with 2MASS and WISE NIR
photometry and high-resolution imaging surveys. We found that NIR and optical
excesses are correlated in multiple NIR photometric bands, suggesting that they
are closely related, likely because more massive disks have higher inner dust
disk walls and are also associated with higher accretion rates. We also found
that multiplicity has no impact on accretion or inner disk properties in a
sample with a wide range of separations, but the sample was too small to
specifically investigate close binaries, where the effects of multiplicity on
disk properties should be most significant.
