  Using SpeX at the NASA Infrared Telescope Facility and the Spitzer Infrared
Spectrograph, we have obtained infrared spectra from 0.7 to 30um for three
young brown dwarfs in the TW Hydra Association (~10 Myr), 2M J1207-3932, 2M
J1139-3159, and SS J1102-3431. The spectral energy distribution for 2M
J1139-3159 is consistent with a stellar photosphere for the entire wavelength
range of our data while the other two objects exhibit significant excess
emission at >5um. We are able to reproduce the excess emission from each brown
dwarf using our models of irradiated accretion disks. According to our model
fits, both disks have experienced a high degree of dust settling. We also find
that silicate emission at 10 and 20um is absent from the spectra of these
disks, indicating that grains in the upper disk layers have grown to sizes
larger than ~5um. Both of these characteristics are consistent with previous
observations of decreasing silicate emission with lower stellar masses and
older ages. These trends suggest that either 1) the growth of dust grains, and
perhaps planetesimal formation, occurs faster in disks around brown dwarfs than
in disks around stars, or 2) the radii of the mid-IR-emitting regions of disks
are smaller for brown dwarfs than for stars, and grains grow faster at smaller
disk radii. Finally, we note the possible detection of an unexplained emission
feature near 14um in the spectra of both of the disk-bearing brown dwarfs.
