Abstract

Whilst the formation of planets continues to have many unknowns, the recent theory of pebble accretion has unveiled a pathway through which the formation of planets can be accelerated compared to the standard core accretion model. These pebbles are of particular interest given recent imaging with ALMA, highlighting rings and other disk substructures in the dust. Here I explore the motion of dust and gas in protoplanetary disks with massive embedded planets using 3D hydrodynamic simulations. In particular, I investigate the consequences of planetary masses above the so-called pebble isolation mass on the dust and gas behaviour. I will go on to broadly speak about the importance of these results on resulting disk and planet compositions.

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