Figure 6 from The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet

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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 6.

Dust continuum emission maps for cases with h/r = 0.05 (left panels), h/r = 0.07 (middle panels), and h/r = 0.1 (right panels) at 1.27 mm. The initial gas surface density at the planet position Σ_g,0 is 3 g cm⁻². The initial dust size distribution is assumed to follow n(s) ∝ s^−3.5 with the maximum grain size of 0.1 mm (DSD1). The layout is the same as that of Figure 1. The images are convolved with a Gaussian kernel with σ of 0.06 r_p (or FWHM of 0.14 r_p), which is shown in the bottom right of the panels.

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