Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud

Measuring the properties of protoplanetary disks around brown dwarfs (BDs) is central to understanding the formation of BDs and their planetary companions. We present modeling of CFHT Tau 4 and 2M0444, two BDs with protoplanetary disks in the Taurus Molecular Cloud. By combining modeling of the spectral energy distributions and Atacama Large Millimeter/submillimeter Array images, we obtain disk radii and masses for these objects; these parameters can be used to constrain BD formation and planet formation, respectively. We find that the disk around CFHT Tau 4 has a total mass of 0.42 MJup and a radius of 80 au; we find 2M0444's disk to have a mass of 2.05 MJup and a radius of 100 au. These radii are more consistent with those predicted by theoretical simulations of BD formation via undisturbed condensation from a mass reservoir than with those predicted by ejection from the formation region. Furthermore, the disk mass of 2M0444 suggests that planet formation may be possible in this disk, although the disk of CFHT Tau 4 is likely not massive enough to form planets. The disk properties measured here provide constraints to theoretical models of BD formation and the formation of their planetary companions.