Kavli Affiliate: Ruobing Dong
| First 5 Authors: Pinghui Huang, Fangyuan Yu, Eve J. Lee, Ruobing Dong, Xue-Ning Bai
| Summary:
From the survival of dust disks for a few Myr to the establishment of
chemical dichotomy, dust traps are expected to play a pivotal role in sculpting
protoplanetary disks and the early planet formation process. These traps
however may not be perfect as evidenced by the detection of gas and dust inside
the gaps and cavities of structured disks. Using two-fluid hydrodynamic global
simulations in both two-dimensions (2D) and three-dimensions (3D), we directly
compute the dynamics of dust grains as they aerodynamically interact with the
disk gas that is being perturbed by an embedded planet of varying mass. In both
2D and 3D, we find the dust trap to be more leaky for lower mass planet and for
higher turbulent $alpha$. More crucially, we find the fraction of the dust
mass that remain trapped within the pressure bump can be up to an order of
magnitude more reduced in 3D vs. 2D with all else equal. Our simulations show a
complex behavior of dust radial motion that is both azimuthally and poloidally
non-uniform, with the overall dynamics dominated by the dust coupling to the
gas flow even for relatively high St = 0.1. The leaky traps we find suggest
pebble isolation mass is likely not truly isolating and that gap-opening
planets do not establish as an unconditional impermeable barrier. Our findings
have implications for recent JWST MINDS results, which show that volatiles,
including water, are present in the inner regions of disks hosting outer dust
rings.
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