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Trapping dust particles in the outer regions of protoplanetary disks
Astronomy and Astrophysics
In order to explain grain growth to mm sized particles and their retention in outer regions of protoplanetary disks, as it is observed at sub-mm and mm wavelengths, we investigate if strong inhomogeneities in the gas density profiles can slow down excessive radial drift and can help dust particles to grow. We use coagulation/fragmentation and disk-structure models, to simulate the evolution of dust in a bumpy surface density profile which we mimic with a sinusoidal disturbance. For differentdoi:10.1051/0004-6361/201118204 fatcat:rq5v44lkvbebhjzsnoiz5st6ue