Main difference compared to most prior work: we use small domains and force fluid turbulence with specified properties. This allows 10-100x better spatial resolution, at the expense of capturing large-scale structure in the turbulence (which may well be important).
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Big picture: I still think the streaming instability is the best candidate planetesimal formation mechanism. But both analytic and simulation evidence now suggests that while the streaming instability is unavoidable, reaching conditions for gravitational collapse is non-trivial.
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Planetesimal formation may need a chain of processes to concentrate solid material: zonal flows, vortices, the streaming instability... If so, the efficiency goes down (may be OK observationally), and there may be places where planetesimals can't form at all.
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