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The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation

  • Authors: Shangjia Zhang, Zhaohuan Zhu, Jane Huang, Viviana V. Guzmán, Sean M. Andrews, Tilman Birnstiel, Cornelis P. Dullemond, John M. Carpenter, Andrea Isella, Laura M. Pérez, Myriam Benisty, David J. Wilner, Clément Baruteau, Xue-Ning Bai, and Luca Ricci

2018 The Astrophysical Journal Letters 869 L47.

  • Provider: AAS Journals

Caption: Figure 10.

“Normalized” radial intensity profile for cases with h/r = 0.05 (left panels) h/r = 0.07 (middle panels), and h/r = 0.1 (right panels). From left to right in each panel block, α = 10−4, 10−3, 10−2 in disks. From top to bottom, the planet mass increases (the layout is similar to Figures 1, 6, and 7). The solid curves are calculated with the DSD1 dust size distribution, while the dotted–dashed curves are calculated with the DSD2 dust size distribution. The seven colors of lines denote different initial gas surface densities (Σg,0). The profiles are smoothed with a Gaussian kernel with σ = 0.06 rp.

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