  We present multi-wavelength radio observations obtained with the VLA of the
protoplanetary disk surrounding the young brown dwarf 2MASS J04442713+2512164
(2M0444) in the Taurus star forming region. 2M0444 is the brightest known brown
dwarf disk at millimeter wavelengths, making this an ideal target to probe
radio emission from a young brown dwarf. Thermal emission from dust in the disk
is detected at 6.8 and 9.1 mm, whereas the 1.36 cm measured flux is dominated
by ionized gas emission. We combine these data with previous observations at
shorter sub-mm and mm wavelengths to test the predictions of dust evolution
models in gas-rich disks after adapting their parameters to the case of 2M0444.
These models show that the radial drift mechanism affecting solids in a gaseous
environment has to be either completely made inefficient, or significantly
slowed down by very strong gas pressure bumps in order to explain the presence
of mm/cm-sized grains in the outer regions of the 2M0444 disk. We also discuss
the possible mechanisms for the origin of the ionized gas emission detected at
1.36 cm. The inferred radio luminosity for this emission is in line with the
relation between radio and bolometric luminosity valid for for more massive and
luminous young stellar objects, and extrapolated down to the very low
luminosity of the 2M0444 brown dwarf.
