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Self-consistent Ring Model in Protoplanetary Disks: Temperature Dips and Substructure Formation

  • Authors: Shangjia Zhang, Xiao Hu, Zhaohuan Zhu, and Jaehan Bae

2021 The Astrophysical Journal 923 70.

  • Provider: AAS Journals

Caption: Figure 6.

The midplane temperature of two-population models with ring configurations. From top to bottom, the dust surface density for the small grains at the Gaussian peak are 0.002, 0.02, and 0.2 g cm−2 (the peak density of big grains are 31.6 times higher). From left to right, the Gaussian widths are 20, 10, and 5 au. Blue, orange and green curves represent α = 10−4, 10−3, and 10−2, respectively. The gray dashed lines are the surface densities of small grains and colored dashed lines are those of big grains. The floor density over the peak density is 10−3. The total dust masses are shown in the top-right corner. In each panel, the dust mass depends on α. The total masses are comparable to what are shown in each panel of Figure 5.

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