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Planetesimal Formation under Realistic Gas Dynamics: Dust Concentration in Turbulent and Windy Protoplanetary Disks

  • Authors: Pinghui Huang, Xue-Ning Bai

Pinghui Huang and Xue-Ning Bai 2026 The Astrophysical Journal Letters 1010 .

  • Provider: AAS Journals

Caption: Figure 1.

Linear integral convolution (LIC) visualization of the poloidal (meridional) gas velocity field, normalized by the sound speed (∣vp∣/cs), for the “Fid,” “B5,” and “T1” models at the final simulation snapshot (t = 2000P0). Model names are labeled in the top-left corner of each panel. The poloidal velocity structures in “B3,” “Am3,” and “S2” are qualitatively similar to those in “Fid” and are therefore omitted for clarity. The cyan arrows mark the locations of current sheets, while the cyan dashed ellipses highlight the VSI corrugation and higher-order body modes.

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