Fig. 5: A schematic process diagram illustrating the astrophysical environment that led to microchondrule enrichment in Ryugu.
From: Abundant microchondrules in 162173 Ryugu suggest a turbulent origin for primitive asteroids
Blue arrows show gas flow, red arrows show migration of large dust particles. Dashed lines represent weaker flows. Two scenarios are possible: (1) the outward transport of microchondrules coupled to gas through viscous spreading or turbulent diffusion, and (2) the inwards transport of microchondrules by cycling through meridional and Lindblad torque flows. Concentration of microchondrules is most likely during inwards transport and could be enhanced by concentration of small particles within highly turbulent, low density regions near the Jovian gap. Distances are based on the models of Bodenan et al.38. The figure is based on observations of a protoplanetary disk by Teague et al.47.
