Fig. 11
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Gas (left panels) and dust (right panels) density for a dusty protoplanetary disk for two values of Stokes number at t=20 kyr. For tightly coupled grains (St=0.01, top row), the gas and dust density remains at equilibrium, while for weakly coupled grains (St=1, bottom row), the dust undergoes both clumping and radial drift toward the pressure maximum.
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