Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44

We model substructure in the protoplanetary disks around DoAr 44 and HD 163296 order to better understand conditions under which planets may form. match archival millimeter-wavelength thermal emission against models of disks' structure that are radiation balance with starlight heating vertical hydrostatic equilibrium, then compare polarized scattered near-infrared images disks. The millimeter arises interior, while probes outer layers. Our best disk has dust masses $81\pm 13$ $M_\oplus$ inner ring at 68 au $82^{+26}_{-16}$ 102 au, both falling within range estimates from previous studies. total mass $84^{+7.0}_{-3.5}$ $M_\oplus$. Unlike 163296, as yet no detected planets. If central cavity is caused by a planet, planet's must be least 0.5 $M_J$ unlikely greater than 1.6 $M_J$. demonstrate disk's bright offset fainter skirt can formed particles drifting through plausible distribution gas.