Abstract
The majority of young low-mass stars are surrounded by disks, consisted of large reservoirs of gas and dust out of which planetary systems eventually form. In the recent years, high spatial resolution observations of such disks by ALMA have revealed many details that are providing interesting constraints on the disk physics as well as dust dynamics, both of which are essential for understanding planet formation. We carry out high-resolution, 2D and 3D hydrodynamic simulations of global disks, including the effects of dust feedback. We find that disks display a rich variety of behaviors, depending on the mutual interactions of dust and gas. These features include both the quasi-axisymmetric rings and non-asymmetric dust traps which are unstable to several possible instabilities. We also show the effects of a new instability associated with dust rings and its observational signatures. These effects are providing a promising new way to promote the formation of many planetesimals in such disks. We produce synthetic dust emission images using our simulation results and discuss the comparison between simulations and observations.
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