Dust ring and gap formation by gas flow induced by low-mass planets embedded in protoplanetary disks - I. Steady-state model

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Fig. 3

Same as Fig. 2, but with the flow structure obtained from m003-hw01 and St = 10⁻⁴ set for the trajectories. In this figure, the planet-induced gas flow is in the flow-headwind regime (see Sect. 3.2). The 3D structure of the gas flow field is shown in Appendix E.

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